LIGHTCURVE PHOTOMETRY OPPORTUNITIES: 2020 JANUARY-MARCH

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 using lightcurve inversion. We also include lists of objects that will or might be radar targets. 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 2020 January-March

In the first three sets of tables, “Dec” is the declination and “U” is the quality code of the lightcurve. See the latest asteroid lightcurve data base (LCDB; Warner et al., 2009; Icarus 202, 134–146.) 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 ≤ 18.0 during any month in the current year and up to five years in the future, e.g., limiting the results by magnitude and declination, family, and more.

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 database. This can be accessed for uploading and downloading data at

http://www.alcdef.org

Containing almost 3.6 million observations for 14840 objects (2019 Oct 6), we believe this to be the largest publicly available database of raw asteroid time-series lightcurve data.

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 and brighter (sometimes 15.0 when the list has too many potential targets).

Lightcurve/Photometry Opportunities

Objects with U = 3– or 3 are excluded from this list since they will likely appear in the list 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 highly-rated result 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.

An entry in bold italics is a near-Earth asteroid (NEA).

		Brightest				LCDB Data
Number	Name	Date		Mag	Dec	Period	Amp	U
3467	Bernheim	01	05.9	15.1	+23
4750	Mukai	01	06.5	15.5	+24	38.3	0.40	2
87135	2000 NU5	01	09.5	15.5	+13		0.76
4540	Oriani	01	13.2	15.2	+14
64163	2001 TB49	01	15.3	15.3	+17
946	Poesia	01	16.4	13.8	+23	108.5	0.24–0.32	2+
18172	2000 QL7	01	20.6	15.4	+68
3759	Piironen	01	21.0	14.7	+17	409.848	0.09–0.56	2
7118	Kuklov	01	21.2	15.5	−1		0.45
437316	2013 OS3	01	21.5	14.8	+25
2075	Martinez	01	21.6	14.2	+30	4.755	0.28	2
1932	Jansky	01	29.5	15.3	+15
6141	Durda	01	30.1	15.4	−2	460.	0.50	2+
3999	Aristarchus	01	30.4	14.8	+17	12.58	0.30	2+
1579	Herrick	01	30.7	15.0	+8
46875	1998 QD104	01	31.4	15.5	+16	88.734	0.47	2
5626	1991 FE	02	02.3	15.1	+11	133.6	0.07–0.44	2
3118	Claytonsmith	02	03.1	14.9	+14	15.794	0.40	2
1678	Hveen	02	04.1	14.9	+26	5.987	0.07	2
2859	Paganini	02	06.7	14.9	+13
5824	Inagaki	02	08.7	15.1	+7
4931	Tomsk	02	11.0	14.8	+4	7.02	0.46	2
3566	Levitan	02	12.0	14.9	+12
163373	2002 PZ39	02	12.0	14.3	+29
4904	Makio	02	15.8	14.9	−5	7.83	0.08	2
2361	Gogol	02	19.0	15.5	+14
4194	Sweitzer	02	20.6	15.3	+10
4705	Secchi	02	20.8	15.2	+10
10419	1998 XB4	02	23.1	15.3	+9
10143	Kamogawa	02	23.8	15.2	−1		0.09
3088	Jinxiuzhonghua	02	26.3	15.4	+5	6.005	0.31	2
3471	Amelin	02	28.9	15.5	+6
2452	Lyot	03	02.8	15.3	+13
1389	Onnie	03	02.9	15.3	+6	22.5	0.34	2
5377	Komori	03	05.1	15.5	+5
5972	Harryatkinson	03	05.7	15.1	+10
1415	Malautra	03	11.2	14.1	+1	>12.	0.03	1
1755	Lorbach	03	11.2	14.8	+7
5070	Arai	03	12.3	15.4	+1	53.	0.30	2
4227	Kaali	03	14.7	15.3	+5
16704	1995 ED8	03	15.1	15.1	−1
1628	Strobel	03	16.7	13.9	−1	9.52	0.20–0.22	2
4570	Runcorn	03	16.9	14.8	+0	>20.	0.12	2-
2905	Plaskett	03	19.7	15.3	+3
38079	1999 HF	03	21.2	15.5	−2
7717	Tabeisshi	03	24.0	15.4	−8
7084	1991 BR	03	27.9	15.4	+0	5.308	0.19	2
1179	Mally	03	29.6	15.3	−4	46.692	0.08	1
331471	1984 QY1	03	29.7	15.3	+6	45.5	0.46–0.65	2
949	Hel	03	31.0	13.0	−17	8.215	0.13–0.14	2+

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 to get more details about a specific asteroid.

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

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 difficult. Refer to Harris et al. (1989; Icarus 81, 365–374) 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 significantly different values for both H and G versus when using average light, which is the method used for values listed by the Minor Planet Center.

The International Astronomical Union (IAU) has adopted a new system, H-G₁₂, introduced by Muinonen et al. (2010; Icarus 209, 542–555). It will be some years before H-G₁₂ becomes widely used. Furthermore, it still needs refinement. That can be done mostly by having data for more asteroids, but only if at very low and moderate phase angles. We strongly encourage obtaining data every degree between 0° to 7°, the non-linear part of the curve that is due to the opposition effect. At angles a > 7°, well-calibrated data every 2° or so out to about 25–30°, if possible, should be sufficient. Coverage beyond about 50° is not generally helpful since the H-G system is best defined with data from 0–30°.

Num	Name	Date		α	V	Dec	Period	Amp	U
389	Industria	01	02.3	0.18	11.0	+23	8.53	0.18–0.34	3
1196	Sheba	01	02.9	0.18	13.5	+23	6.319	0.21–0.28	3
412	Elisabetha	01	04.5	0.44	12.8	+22	19.635	0.08–0.20	3
1292	Luce	01	04.7	0.33	14.1	+22	6.954	0.17–0.26	3
1010	Marlene	01	04.9	0.18	14.4	+23	31.06	0.17–0.32	2+
222	Lucia	01	06.7	0.36	14.0	+24	7.837	0.25–0.41	3
498	Tokio	01	06.9	0.73	12.8	+25	41.85	0.23–0.23	3
407	Arachne	01	13.0	0.21	12.1	+22	22.627	0.30–0.31	3
946	Poesia	01	16.4	0.61	13.8	+23	108.5	0.24–0.32	2+
274	Philagoria	01	20.0	0.79	14.1	+23	17.938	0.37–0.51	3
863	Benkoela	01	20.9	0.69	13.4	+22	8.20	0.05–0.27	3-
537	Pauly	01	21.1	0.04	13.9	+20	16.168	0.14–0.20	3
112	Iphigenia	01	30.9	0.35	13.2	+19	31.466	0.30	3
816	Juliana	02	01.6	0.62	13.8	+19	10.557	0.22–0.53	3
860	Ursina	02	02.3	0.38	14.4	+16	9.386	0.22–0.50	3
1274	Delportia	02	03.6	0.86	14.0	+18	5.615	0.05–0.26	3
1503	Kuopio	02	04.1	0.41	13.1	+17	9.957	0.65–0.90	3
622	Esther	02	08.0	0.38	12.9	+14	47.5	0.30–0.6	2
1266	Tone	02	08.1	0.26	14.1	+16	7.40	0.06–0.12	2
90	Antiope	02	17.0	0.80	13.3	+15	16.509	0.05–0.88	3
227	Philosophia	02	20.1	0.36	13.0	+10	26.468	0.06–0.20	3
231	Vindobona	02	20.4	0.84	13.6	+14	14.245	0.20–0.29	3
46	Hestia	02	21.6	0.59	12.2	+09	21.040	0.09–0.12	3
602	Marianna	02	22.2	0.17	13.1	+10	35.195	0.07–0.17	3
591	Irmgard	02	24.7	0.24	12.8	+09	7.35	0.23–0.26	3
582	Olympia	02	25.2	0.19	11.2	+09	36.312	0.05–0.6	3
101	Helena	02	25.6	0.67	12.2	+11	23.080	0.09–0.13	3
839	Valborg	02	27.9	0.05	14.5	+08	10.366	0.14–0.19	3
30	Urania	02	29.6	0.74	10.6	+06	13.686	0.11–0.45	3
66	Maja	03	01.3	0.78	12.9	+09	9.735	0.21–0.45	3
538	Friederike	03	04.0	0.94	14.5	+10	46.728	0.25–0.25	3
184	Dejopeja	03	06.4	0.20	12.2	+05	6.442	0.22–0.3	3
358	Apollonia	03	08.8	0.16	13.0	+04	50.6	0.15–0.15	3−
124	Alkeste	03	09.5	0.61	11.3	+03	9.906	0.08–0.30	3
122	Gerda	03	09.8	0.15	12.1	+04	10.685	0.10–0.26	3
477	Italia	03	16.0	0.75	13.9	+04	19.413	0.15–0.32	3
271	Penthesilea	03	16.2	0.55	14.2	+00	18.787	0.23–0.33	3
1628	Strobel	03	16.8	0.91	13.9	−01	9.52	0.20–0.22	2
569	Misa	03	19.7	0.68	13.4	−01	11.595	0.09–0.25	3
277	Elvira	03	24.5	0.41	14.1	−03	29.69	0.34–0.59	3
1225	Ariane	03	28.8	0.22	14.1	−03	5.507	0.30–0.36	3
2616	Lesya	03	31.0	0.76	14.9	−03	9.217	0.43–0.51	3
300	Geraldina	03	31.1	0.17	14.4	−04	6.842	0.04–0.32	3
671	Carnegia	03	31.7	0.71	14.4	−06	8.332	0.24	3−

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

Additional lightcurves 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.

Favorable apparitions are in bold text. NEAs are in italics.

		Brightest				LCDB Data
Num	Name	Date		Mag	Dec	Period	Amp	U
118	Peitho	01	02.7	11.3	+35	7.8055	0.11–0.33	3
1292	Luce	01	04.8	14.1	+22	6.9541	0.17–0.26	3
4374	Tadamori	01	05.6	14.8	+15	4.5047	0.77–0.94	3
81	Terpsichore	01	12.6	11.7	+33	10.943	0.06–0.10	3
545	Messalina	01	13.1	14.2	+32	7.2	0.22–0.27	3
368	Haidea	01	14.8	15.1	+11	9.823	0.15–0.23	3
1670	Minnaert	01	15.2	15.0	+35	3.528	0.23–0.25	3
198	Ampella	01	15.5	11.8	+14	10.379	0.11–0.22	3
755	Quintilla	01	16.9	14.3	+17	4.552	0.08–0.45	3
131	Vala	01	18.1	13.1	+27	5.1812	0.08–0.32	3
6084	Bascom	01	18.4	15.2	−2	2.7454	0.14–0.23	3
815	Coppelia	01	19.9	14.2	+40	4.421	0.17–0.24	3
766	Moguntia	01	20.0	14.1	+34	4.8164	0.06–0.23	3
2105	Gudy	01	25.7	14.4	−15	15.795	0.18–0.52	3−
598	Octavia	01	28.6	13.4	+29	10.8903	0.05–0.28	3
456	Abnoba	01	29.8	13.4	−2	18.281	0.2–0.32	3
643	Scheherezade	01	30.5	14.4	+1	14.161	0.23–0.37	3
1845	Helewalda	01	30.5	14.8	+14	7.2786	0.15–0.34	3−
481	Emita	01	31.8	12.3	+31	14.412	0.16–0.30	3
1052	Belgica	02	02.1	14.4	+21	2.7097	0.08–0.10	3
860	Ursina	02	02.3	14.4	+16	9.386	0.22–0.50	3
76818	2000 RG79	02	02.9	15.4	+1	3.1664	0.14–0.15	3
1689	Floris–Jan	02	07.8	14.9	+18	145.	0.02– 0.4	3
3511	Tsvetaeva	02	08.0	15.0	+0	6.2279	0.80–0.92	3
503	Evelyn	02	10.4	12.0	+22	38.78	0.30– 0.5	3−
195	Eurykleia	02	11.5	12.7	+22	16.521	0.10–0.24	3
40267	1999 GJ4	02	13.4	14.3	−25	4.9567	0.67–1.11	3
267	Tirza	02	13.7	14.3	+22	7.648	0.18– 0.4	3
35107	1991 VH	02	15.5	15.2	+19	2.6236	0.08–0.15	3
4031	Mueller	02	16.4	15.0	+32	2.942	0.14–0.19	3
205	Martha	02	17.0	13.3	−2	14.911	0.10–0.50	3
1308	Halleria	02	19.2	14.6	+15	6.028	0.14–0.17	3
782	Montefiore	02	19.4	13.5	+20	4.0728	0.31–0.54	3
1967	Menzel	02	19.6	14.7	+18	2.835	0.24–0.39	3
2151	Hadwiger	02	24.2	14.4	+29	5.872	0.07–0.38	3
101	Helena	02	25.6	12.2	+11	23.08	0.09–0.13	3
1604	Tombaugh	02	27.4	15.1	+2	7.24	0.16–0.35	3−
839	Valborg	02	28.0	14.5	+8	10.366	0.14–0.19	3
619	Triberga	03	02.7	13.6	−2	29.311	0.30–0.45	3
5175	Ables	03	04.8	15.5	−22	2.798	0.06–0.10	3
1016	Anitra	03	05.6	14.4	+10	5.9295	0.26–0.50	3
3497	Innanen	03	07.9	14.8	+7	7.181	0.39–0.60	3
7132	Casulli	03	08.3	15.1	+0	3.524	0.15–0.25	3−
987	Wallia	03	08.8	14.9	+0	10.0813	0.11–0.36	3
124	Alkeste	03	09.6	11.3	+3	9.906	0.08–0.30	3
2903	Zhuhai	03	12.8	15.0	−16	5.263	0.32–0.54	3
1139	Atami	03	13.6	14.7	−13	27.446	0.15–0.45	3
78	Diana	03	15.8	10.6	−4	7.2991	0.02–0.30	3
477	Italia	03	16.1	13.9	+4	19.413	0.15–0.32	3
3223	Forsius	03	17.5	14.3	+4	2.343	0.20–0.28	3
4175	Billbaum	03	19.1	15.2	+6	2.73	0.08–0.15	3−
939	Isberga	03	21.0	15.3	−2	2.9173	0.20–0.25	3
651	Antikleia	03	22.5	14.7	+8	20.299	0.13–0.41	3
6382	1988 EL	03	23.4	14.8	−12	2.895	0.06–0.20	3
901	Brunsia	03	25.8	14.7	−7	3.1363	0.09–0.28	3
217	Eudora	03	27.5	14.4	+3	25.272	0.08–0.31	3
1225	Ariane	03	28.8	14.1	−3	5.5068	0.30–0.36	3
909	Ulla	03	30.1	14.6	+12	8.73	0.08–0.24	3
300	Geraldina	03	31.1	14.4	−4	6.8423	0.04–0.32	3
850	Altona	03	31.6	13.7	+17	11.1913	0.09–0.17	3
420	Bertholda	03	31.8	13.1	−11	11.04	0.24–0.29	3

Radar-Optical Opportunities

Past radar targets:

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

Arecibo targets:

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

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

Goldstone targets:

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

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 the Minor Planet Center observing tools

In particular, monitor NEAs 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 or their Facebook or Twitter accounts) if you get data. The team may not always be observing the target but 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 circle distances (in degrees) of the Sun and Moon from the asteroid. MP is the lunar phase and GB is the galactic latitude. “PHA” 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.

About YORP Acceleration

Many, if not all, of the targets in this section are near-Earth asteroids. These objects are particularly sensitive to YORP acceleration. YORP (Yarkovsky–O’Keefe–Radzievskii–Paddack) is the asymmetric thermal re-radiation of sunlight that can cause an asteroid’s rotation period to increase or decrease. High precision lightcurves at multiple apparitions can be used to model the asteroid’s sidereal rotation period and see if it’s changing.

It usually takes four apparitions to have sufficient data to determine if the asteroid rotation rate is changing under the influence of YORP. This is why observing asteroids that already have well-known periods remains a valuable use of telescope time. It is even more so when considering the BYORP (binary-YORP) effect among binary asteroids that has stabilized the spin so that acceleration of the primary body is not the same as if it would be if there were no satellite.

To help focus efforts in YORP detection, Table I gives a quick summary of this quarter’s radar-optical targets. The family or group for the asteroid is given under the number name. Also under the name will be additional flags such as “PHA” for Potentially Hazardous Asteroid, NPAR for a tumbler, and/or “BIN” to indicate the asteroid is a binary (or multiple) system. “BIN?” means that the asteroid is a suspected but not confirmed binary. The period is in hours and, in the case of binary, for the primary. The Amp column gives the known range of lightcurve amplitudes. The App columns gives the number of different apparitions at which a lightcurve period was reported while the Last column gives the year for the last reported period. The R SNR column indicates the estimated radar SNR using the tool at

Table I.

Summary of radar-optical opportunities for the current quarter. Period and amplitude data are from the asteroid lightcurve database (Warner et al., 2009; Icarus 202, 134–146). SNR values are estimates that are affected by radar power output along with rotation period, size, and distance. They are given for relative comparisons among the objects in the list.

Asteroid	Period	Amp	App	Last	R	SNR
(437316) 2013 OS3	–	–	–	–	A	32
NEA					G	–
2012 RK15	–	–	–		A	260
NEA					G	90
(163373) 2002 PZ39	–	–	–	–	A	800
NEA					G	270
(35107) 1991 VH	2.623	0.08	5	2014	A	–
NEA BIN		0.15			G	–
2011 EH	–	–	–	–	A	890
NEA					G	300
2017 BM123	2.150	0.37	1	2017	A	105
NEA NHATS					G	35
2015 RH2	–	–	–	–	A	7
NEA NHATS					G	–
(65690) 1991 DG	–	–	–	–	A	35
NEA					G	–

http://www.naic.edu/~eriverav/scripts/index.php

The “A” is for Arecibo; “G” is for Goldstone.

The SNRs were calculated using the current MPCORB absolute magnitude (H), a period of 4 hours (2 hours if D ≤ 200 m) if it’s not known, and the approximate minimum Earth distance during the current quarter. These are estimates only and assume that the radars are fully functional.

If the SNR value is in bold text, the object was found on the radar planning pages listed above. Otherwise, the planning tool at

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

was used to find known NEAs that were V < 18.0 during the quarter. An object is usually placed on the list only if the estimated Arecibo SNR > 10 when using the SNR calculator mentioned above.

It’s rarely the case, especially when shape/spin axis modeling, that there are too much data. Remember that the best set for modeling includes data not just from multiple apparitions but from as wide a range of phase angles during each apparition as well.

(437316) 2013 OS3 (H = 18.4)

There are no periods reported in the LCDB. The estimated diameter is about 600 meters, so the rotation period will likely be > 2 hours. The asteroid starts the year not far from the North Celestial Pole but quickly moves south and crosses the equator towards the end of January.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
01/01	08	17.0	+67	08	0.27	1.18	17.4	37.1	134	116	+0.30	+33
01/05	07	53.9	+64	50	0.23	1.16	16.9	35.4	137	80	+0.67	+31
01/09	07	26.7	+60	53	0.19	1.14	16.4	32.7	141	43	+0.96	+28
01/13	06	57.3	+54	09	0.15	1.11	15.8	29.0	147	48	−0.93	+23
01/17	06	27.9	+42	50	0.12	1.09	15.2	25.1	152	101	−0.56	+14
01/21	06	00.6	+24	59	0.10	1.07	14.8	27.3	150	164	−0.15	+1
01/25	05	36.6	+01	52	0.10	1.06	15.1	41.2	135	133	+0.00	−16
01/29	05	16.3	−19	34	0.11	1.04	15.8	57.8	117	81	+0.15	−29
02/02	04	59.5	−34	49	0.13	1.02	16.5	69.7	103	56	+0.50	−37
02/06	04	45.3	−44	46	0.16	1.01	17.2	76.8	94	71	+0.86	−41

2012 RK15 (H = 23.4)

The observing window for those with modest telescopes is just more than a week for this 60-m NEA. The rotation period is unknown but keep in mind that the chances are good that the period is < 2 hours.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
01/28	02	20.3	+33	09	0.02	0.99	18.1	82.2	96	65	+0.09	−26
01/29	04	10.6	+38	52	0.02	1.00	17.5	60.5	118	76	+0.15	−9
01/30	05	45.9	+38	20	0.03	1.01	17.4	43.0	136	83	+0.23	+5
01/31	06	48.0	+35	16	0.04	1.01	17.5	31.3	148	84	+0.31	+15
02/01	07	26.4	+32	10	0.04	1.02	17.7	23.8	155	80	+0.40	+21
02/02	07	51.2	+29	38	0.05	1.03	18.0	19.0	160	73	+0.50	+25
02/03	08	08.2	+27	39	0.06	1.04	18.2	15.7	163	65	+0.59	+28
02/04	08	20.4	+26	05	0.07	1.05	18.5	13.5	166	55	+0.69	+30
02/05	08	29.6	+24	50	0.08	1.06	18.7	12.0	167	45	+0.78	+32
02/06	08	36.8	+23	50	0.09	1.07	18.9	11.0	168	33	+0.86	+33

(163373) 2002 PZ39 (H = 18.9)

The diameter is ~500 m, but the close approach of 0.04 AU or 16 LD (lunar distances) allows it to be worked with modest telescopes. It brightens slowly the second half of January but then, after closest approach on Feb 12, the viewing circumstances soon become unfavorable. The period should be > 2 hours.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
01/10	09	12.4	+19	41	0.36	1.31	18.2	19.1	154	36	+0.99	+40
01/15	09	10.3	+20	01	0.30	1.27	17.7	15.6	160	36	−0.78	+39
01/20	09	05.9	+20	32	0.25	1.23	17.0	11.4	166	108	−0.24	+38
01/25	08	58.0	+21	19	0.20	1.18	16.3	6.5	172	174	+0.00	+37
01/30	08	44.2	+22	30	0.15	1.14	15.5	4.0	175	122	+0.23	+34
02/04	08	18.3	+24	23	0.11	1.09	15.0	12.5	166	55	+0.69	+29
02/09	07	19.4	+27	20	0.07	1.05	14.5	30.1	148	28	+1.00	+18
02/14	04	29.6	+26	42	0.04	1.00	14.5	72.4	105	139	−0.71	−15

(35107) 1991 VH (H = 16.7; Binary/Trinary)

Pravec et al. (1997; IAUC 6607) reported this as a binary asteroid with a primary period of 2.624 h and orbital period of 32.69 h. Reanalysis of data from 2003 (Pravec et al., 2006; Icarus 181, 63–93) found three periods, indicating the possibility of a second satellite. This is a prime target for a coordinated campaign with observers well-spaced around the globe. Also required will be high-quality data with < 0.02 mag accuracy and precision. There is good news: 1991 VH is within easy reach throughout the first quarter of 2020.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
01/01	10	40.4	−07	25	0.44	1.23	17.1	46.7	114	160	+0.30	+43
01/11	10	46.5	−04	43	0.39	1.25	16.7	40.7	124	53	−1.00	+46
01/21	10	47.0	−00	16	0.35	1.26	16.3	32.6	136	91	−0.15	+49
01/31	10	40.6	+06	11	0.32	1.27	15.8	22.1	151	141	+0.31	+53
02/10	10	27.5	+14	17	0.30	1.28	15.3	10.4	166	3	−0.99	+54
02/20	10	09.7	+22	40	0.31	1.29	15.3	8.7	169	142	−0.12	+53
03/01	09	51.4	+29	39	0.33	1.30	15.9	19.4	154	91	+0.33	+51
03/11	09	37.6	+34	25	0.37	1.30	16.4	29.1	140	54	−0.97	+48
03/21	09	30.8	+37	07	0.42	1.30	16.9	36.6	129	160	−0.10	+47
03/31	09	31.3	+38	16	0.47	1.30	17.3	42.0	119	53	+0.36	+47

2011 EH (H = 25.5)

The estimated diameter is only 25 meters, meaning that there is a good chance of 2011 EH being a super-fast rotator. Sky motion will be fast, reaching 107″/min around Feb 18 at 00:00 UT.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
02/17	18	56.2	+24	53	0.01	0.98	20.5	121.3	58	56	−0.38	+10
02/18	15	45.3	+32	24	0.01	0.99	18.1	79.2	100	61	−0.28	+52
02/19	13	13.1	+25	08	0.01	1.00	17.8	45.3	134	91	−0.20	+85
02/20	12	09.8	+18	28	0.02	1.00	18.2	29.1	150	114	−0.12	+77
02/21	11	40.0	+14	38	0.03	1.01	18.6	20.7	159	132	−0.06	+69
02/22	11	23.2	+12	19	0.03	1.02	19.0	15.5	164	148	−0.03	+65
02/23	11	12.5	+10	47	0.04	1.03	19.3	12.0	168	162	+0.00	+62
02/24	11	05.1	+09	42	0.05	1.04	19.5	9.3	170	175	+0.00	+59

2017 BM123 (H = 23.7; NHATS)

Warner (MPB 44, 223–237) reported a secure period of 2.150 h for this 50-meter NEA based on observations in 2017. That is the only entry in the LCDB. The observing window is only about 10 days. Fortunately, the moon won’t be much of a problem.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
02/20	09	45.9	+10	01	0.06	1.05	18.0	5.8	174	144	−0.12	+43
02/22	09	53.7	+14	57	0.05	1.04	17.7	7.0	173	169	−0.03	+47
02/24	10	05.3	+21	48	0.04	1.03	17.6	12.4	167	166	+0.00	+52
02/26	10	24.1	+31	23	0.03	1.02	17.5	21.6	158	142	+0.05	+58
02/28	10	58.5	+44	23	0.03	1.01	17.5	35.2	144	118	+0.17	+62
03/01	12	12.7	+59	18	0.03	1.01	17.8	52.8	126	98	+0.33	+57
03/03	14	56.9	+68	31	0.03	1.00	18.4	71.5	107	88	+0.52	+45

2015 RH2 (H = 21.9; NHATS)

The main reason this asteroid is included is because it’s a potential target for a human mission. Visit https://cneos.jpl.nasa.gov/nhats/ for information and observing tools under the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) program. The estimated size is only 12 meters, so be alert for this being a super-fast rotator. Keep in mind the rule of thumb that exposures must be < 0.187P (period) to avoid rotational smearing.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
02/20	14	22.1	−17	22	0.09	1.03	19.1	63.5	112	71	−0.12	+40
02/23	14	05.0	−18	52	0.10	1.04	19.0	57.3	118	110	+0.00	+41
02/26	13	48.5	−20	05	0.10	1.05	19.0	51.4	124	147	+0.05	+41
02/29	13	32.7	−21	00	0.11	1.06	19.0	45.8	130	163	+0.24	+41
03/03	13	17.6	−21	38	0.12	1.08	19.0	40.5	135	130	+0.52	+41
03/06	13	03.3	−22	01	0.12	1.09	19.0	35.6	140	89	+0.81	+41
03/09	12	50.0	−22	10	0.13	1.10	19.0	31.0	145	46	+0.99	+41
03/12	12	37.7	−22	07	0.14	1.12	19.0	26.9	150	22	−0.92	+41
03/15	12	26.4	−21	54	0.15	1.13	19.1	23.2	153	55	−0.65	+41
03/18	12	16.2	−21	32	0.16	1.14	19.2	20.2	157	94	−0.34	+41

(65690) 1991 DG (H = 19.0)

At 470 meters, this NEA is a “giant” compared to some others this quarter. The observing window extends from mid-February to early April. Weather permitting, it should be possible to get data at more than one lunation, which will be a great help for modeling.

DATE	RA		Dec		ED	SD	V	α	SE	ME	MP	GB
02/10	10	18.7	−14	54	0.36	1.31	18.5	23.5	148	30	−0.99	+34
02/20	10	10.9	−14	11	0.28	1.25	17.7	19.9	155	125	−0.12	+33
03/01	09	58.1	−11	12	0.22	1.19	17.0	18.6	157	103	+0.33	+33
03/11	09	40.2	−04	28	0.16	1.14	16.4	23.8	152	45	−0.97	+34
03/21	09	15.8	+08	48	0.12	1.09	16.1	38.2	138	168	−0.10	+36
03/31	08	37.3	+32	26	0.09	1.04	16.1	63.1	112	42	+0.36	+35
04/10	06	58.5	+62	23	0.09	0.99	17.0	94.0	81	116	−0.94	+25

IN THIS ISSUE

This list gives those asteroids in this issue for which physical observations (excluding astrometric only) were made. This includes lightcurves, color index, and H-G determinations, etc. In some cases, no specific results are reported due to a lack of or poor quality data. The page number is for the first page of the paper mentioning the asteroid. EP is the “go to page” value in the electronic version.

Number	Name	EP	Page
33	Polyhymnia	34	34
206	Hersilia	34	34
243	Ida	13	13
289	Nenetta	61	61
395	Delia	34	34
400	Ducrosa	34	34
472	Roma	61	61
624	Hektor	43	43
635	Vundtia	61	61
855	Newcombia	50	50
855	Newcombia	75	75
869	Mellena	61	61
874	Rotraut	13	13
900	Rosalinde	34	34
1066	Lobelia	34	34
1268	Libya	37	37
1355	Magoeba	50	50
1355	Magoeba	75	75
1435	Garlena	20	20
1466	Mundleria	13	13
1583	Antilochus	43	43
1605	Milankovitch	7	7
1620	Geographos	23	23
1686	De Sitter	13	13
1727	Mette	50	50
1727	Mette	75	75
1802	Zhang Heng	7	7
1814	Bach	7	7
1865	Cerberus	23	23
1868	Thersites	43	43
2025	Nortia	7	7
2051	Chang	1	1
2059	Baboquivari	23	23
2096	Vaino	18	18
2100	Ra-Shalom	23	23
2131	Mayall	61	61
2150	Nyctimene	50	50
2150	Nyctimene	75	75
2285	Ron Helin	13	13
2302	Florya	13	13
2432	Soomana	50	50
2432	Soomana	75	75
2460	Mitlincoln	5	5
2511	Patterson	50	50
2511	Patterson	75	75
2548	Leloir	64	64
2564	Kayala	7	7
2595	Gudiachvili	7	7
2602	Moore	7	7
2602	Moore	11	11
2920	Automedon	43	43
3070	Aitken	5	5
3122	Florence	3	3
3122	Florence	21	21
3295	Murakami	69	69
3306	Byron	13	13
3549	Hapke	7	7
3709	Polypoites	43	43
3793	Leonteus	43	43
3830	Trelleborg	3	3
4060	Deipylos	43	43
4125	Lew Allen	50	50
4125	Lew Allen	75	75
4148	McCartney	7	7
4148	McCartney	71	71
4495	Dassanowsky	37	37
4501	Eurypylos	43	43
4569	Baerbel	50	50
4569	Baerbel	75	75
4717	Kaneko	74	74
4807	Noboru	20	20
4807	Noboru	71	71
4868	Knushevia	50	50
4868	Knushevia	75	75
4961	Timherder	69	69
5104	Skripnichenko	18	18
5199	Dortmund	13	13
5244	Amphilochos	43	43
5391	Emmons	13	13
5522	De Rop	71	71
5786	Talos	23	23
6161	Vojno-Yasenetsky	7	7
6485	Wendeesther	50	50
6485	Wendeesther	75	75
6527	Takashiito	64	64
6558	Norizuki	50	50
6558	Norizuki	75	75
6843	Heremon	71	71
6901	Roybishop	50	50
6901	Roybishop	75	75
7081	Ludibunda	7	7
7365	Sejong	13	13
7520	1990 BV	71	71
7527	Marples	64	64
7759	1990 QD2	50	50
7759	1990 QD2	75	75
9509	Amfortas	50	50
9509	Amfortas	75	75
9565	Tikhonov	50	50
9565	Tikhonov	75	75