The Minor Planet Bulletin

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BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS

VOLUME 44, NUMBER 1, A.D. 2017 JANUARY-MARCH 1.

EDITORIAL ANNOUNCEMENTS: (http://www.minorplanet.info/minorplanetbulletin.html) along MPB VOLUME 44 with MPB templates in Microsoft Word (Word 97) DOT and Word 2007 and above (DOTX) files. The templates include Richard P. Binzel, Editor instructions for using them as “starter papers” or to import MPB Brian D. Warner, Associate Editor paragraph styles into new or existing Word documents. David Polishook, Assistant Editor

We welcome Dr. David Polishook as a new Assistant Editor and describe a new manuscript submission LIGHTCURVE ANALYSIS FOR requirement of a Summary Table for lightcurve results. THREE MAIN-BELT ASTEROIDS

Stephen M. Brincat As evidenced by the figure below, rapid growth continues for the Flarestar Observatory (MPC 171) Minor Planet Bulletin. Volume 43 (2016) had a record number of San Gwann SGN 3160, MALTA 366 pages and results for more than 700 asteroids. [email protected]

(Received: 2016 August 13)

Photometric observations of three main-belt asteroids were made from 2016 March to June. The results of the lightcurve analysis are reported for 1154 Astronomia (1927 CB), 3680 Sasha (1987 MY), and (6138) 1991 JH1.

The purpose of this research was to obtain the lightcurves of three main-belt asteroids: 1154 Astronomia (1927 CB), 3680 Sasha (1987 MY), and (6138) 1991 JH1 in order to determine the rotation period for each asteroid. A search of the asteroid lightcurve database (LCDB; Warner et al., 2009) and other sources did not find previously reported lightcurve results for these asteroids. Two editorial adjustments are needed to manage this growth. The All observations were obtained at Flarestar Observatory (MPC first is that we welcome Dr. David Polishook of the Weizmann Code: 171) at San Gwann, Malta. A Meade f/6.3 0.25-m Schmidt Institute of Science as a new Assistant Editor. Brian D. Warner Cassegrain Telescope (SCT) coupled to a Moravian G2-1600 continues as an Associate Editor and Professor Richard P. Binzel CCD was used. The pixel scale was 0.99 arcsec/pix at 1x1 as Editor. Dr. Robert A. Werner and Derald D. Nye continue in binning. This provided a field-of-view of 25.6x17.1 arcmin. All their service as MPB Producer and Distributor, respectively. asteroid images were obtained through a clear filter with integration times varying between 180 to 360 seconds depending The second adjustment is a requirement for all submitted on the brightness of the asteroid. All observing sessions were manuscripts, when appropriate, to contain a Summary Table of operated remotely through Sequence Generator Pro (SGP). All results that is constructed using a standard format. The table is images were dark and flat-field corrected. required to facilitate the entry of results into the Asteroid Lightcurve Data Base (LCDB). Lightcurve results manuscripts Differential photometry measurements were made in MPO not containing this Summary Table will be returned to the author. Canopus (Warner, 2015) using the FALC routine (Harris et. al., 1989) to derive the asteroid synodic periods. The StarBGone The table format is fully described in the “Authors Guide” utility in MPO Canopus was applied to measure images when appearing on page 81 of this issue and posted online asteroids where located in the vicinity of stars. The MPO Canopus Minor Planet Bulletin 44 (2017) Available on line http://www.minorplanet.info/mpbdownloads.html 2

Comp Star Selector utility was employed to select comparison 6138 (1991 JH1). This main-belt asteroid was discovered on 1991 stars of near solar-colour for differential photometry for all the May 14 by Otomo and Muramatsu at Kiyosato. It was reported as three asteroids. Information about discovery circumstances were a lightcurve photometry opportunity on the CALL website and obtained from the JPL small bodied Database, (JPL, 2016). All the observed on the nights of 2016 March 27, 30, and April 10. targets were selected from the CALL website (CALL, 2015). Exposures were 240 s for March 27 and 300 s for the remaining nights. Based on 218 data points, the derived synodic period is Observing circumstances and results are summarized in Table I. 5.4578 ± 0.006 h with an amplitude of 0.30 ± 0.09 mag.

1154 Astronomia (1927 CB) was discovered on 1927 February 8 by K. Reinmuth at Heidelberg. The asteroid was observed during eight nights from 2016 May 5 to June 14. Exposures were 300 seconds, except on June 14 when exposures were 360 seconds. A total of 347 data points were used to find the synodic period of 18.1154 ± 0.0139 h and amplitude of 0.39 ± 0.05 mag.

Acknowledgements

I would like to thank Brian Warner his work in the development of MPO Canopus and for his efforts in maintaining the CALL website.

References 3680 Sasha (1987 MY) is a main-belt asteroid that was discovered on 1987 June 28 by E.F. Helin at Palomar. It was reported as a CALL (2015). Collaborative Asteroid Lightcurve Link. lightcurve photometry opportunity on the CALL website and http://www.MinorPlanet.info/call.html observed on four nights in 2016 March. The lightcurve is based on 329 data points with exposures of 180 s. The derived synodic Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., period is 5.8145 ± 0.005 h with an amplitude of 0.30 ± 0.05 mag. Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

JPL (2016). Small-Body Database Browser - JPL Solar System Dynamics web site. http://ssd.jpl.nasa.gov/sbdb.cgi

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid lightcurve database.” Icarus 202, 134-146. Updated 2016 Sept. http://www.MinorPlanet.info/lightcurvedatabase.html

Warner, B.D. (2015). MPO Canopus software v10.7.0.6. Bdw Publishing. http//www.MinorPlanetObserver.com

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 1154 Astronomia 05/05-06/14 347 1.2,12.7 225 3 18.1154 0.0139 0.39 0.05 3680 Sasha 03/05-03/19 329 6.0,2.8,5.9 169 4 5.8145 0.0047 0.30 0.05 6138 1991 JH 03/28-04/10 218 7.5,2.2,2.3 199 3 5.4578 0.0006 0.30 0.09

Table I. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which

is the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude. Minor Planet Bulletin 44 (2017) 3

ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2015 FEBRUARY – MARCH

Kylie Hess, Madison Bruner, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected]

(Received: 2016 September 5)

Photometric data were taken over four nights in 2015 February and one night in 2015 March for six asteroids: 507 Laodica, 583 Klotilde, 1911 Schubart, 2136 Jugta, 4958 Wellnitz, and (70171) 1999 OL2. In 2015 March, data were taken over five nights for 1027 Aesculapia, thirteen nights for 2522 Triglav, seven nights for 2581 Radegast and 4856 Seaborg, twelve nights for 10143 Kamogawa, and six nights for (16029) 1999 DQ6, 3733 Yoshitomo, 4963 Kanroku, and (7588) 1992 FJ1.

Photometric observations of a number of asteroids were made from the Oakley Southern Sky Observatory in New South Wales, Australia, using an f/8.1 0.5-m Ritchey-Chretien telescope and STX-16803 camera, binned 3x3, with a luminance filter. The image scale was 1.344 arcsec/pix. The images were calibrated in MaxIM DL using bias, dark, and twilight flat frames. The images were measured and lightcurves were made using MPO Canopus.

Table I gives the observing circumstances, exposure (seconds), and derived period and amplitude – if found – for each asteroid. The period determined for 507 Laodica matched the period determined by Black et al. (2016) to within experimental error. For the seven objects where a period could not be found, only the amplitude is reported.

References

Black, S., Linville, D. Michalik, D., Wolf, M., Ditteon, R. (2016). “Lightcurve Analysis of Asteroids Observed at the Oakley Southern Sky Observatory: 2015 December – 2016 April.” Minor Planet Bulletin 43, 287-289.

EDITOR’S NOTE: It seems appropriate to add some commemoration to the lightcurve observations of 2136 Jugta presented here and recently by G. B. Casalnuovo (2015; MPB 43, 112). Long-time readers will recall J. U. Gunter (1911-1994), who was a retired pathologist who self-published a bimonthly newsletter named Tonight’s Asteroids in the 1970’s and 80’s. (“JUGTA” is a concatenation of Gunter’s initials and those of his newsletter.) It was Gunter who sparked amateur and professional astronomers’ interest in asteroids (including MPB Staff members Binzel, Werner, Nye and Section Recorder Pilcher). A more detailed description of Gunter’s contributions may be found in MPB 22, page 1 (1995).

Minor Planet Bulletin 44 (2017) 4

Number Name 2015 mm/dd Pts Exp Phase LPAB BPAB Period P.E. Amp A.E. 507 Laodica 02/17-03/09 66 45 3.5,9.8 139 -5 4.7064 0.0007 0.18 0.04 583 Klotilde 02/17-03/09 78 30 4.7,11.0 144 -10 9.2134 0.0012 0.17 0.01 1027 Aesculapia 03/16-03/21 71 120 8.8,10.7 154 1 13.529 0.042 0.09 0.03 1911 Schubart 02/17-03/09 66 150 4.5,10.4 134 -1 - - 0.10 0.05 2136 Jugta 02/17-03/09 67 180 3.2,10.6 140 -1 6.4571 0.0007 0.45 0.05 2522 Triglav 03/11-03/27 248 180 4.5,7.7 170 -11 6.774 0.002 0.29 0.05 2581 Radegast 03/11-03/21 102 180 4.0,9.1 164 -3 8.753 0.002 0.82 0.06 3733 Yoshitomo 03/22-03/27 111 120 5.4,6.4 180 -8 - - 0.06 0.02 4856 Seaborg 03/11-03/21 111 150 3.8,6.6 168 -7 15.853 0.007 0.41 0.06 4958 Wellnitz 02/17-03/09 79 180 5.0,10.8 143 -11 - - 0.14 0.04 4963 Kanroku 03/22-03/27 107 150 3.9,5.7 175 -6 - - 0.10 0.04 7588 1992 FJ1 03/22-03/27 129 180 9.1,8.7 190 -20 - - 0.21 0.04 10143 Kamogawa 03/16-03/27 240 180 9.2,9.9 179 -18 - - 0.09 0.05 16029 1999 DQ6 03/16-03/21 89 180 5.7,7.8 163 -3 5.95 0.01 0.76 0.02 70171 1999 OL2 02/17-03/09 69 180 6.5,17.9 141 -8 - - 0.17 0.07

Table I. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude.

Minor Planet Bulletin 44 (2017) 5

the Sun, instead of opposition. Though unconventional, it has the advantage that many close approaches do not involve actual opposition to the Sun near the time of minimum distance and greatest brightness and are missed by an opposition-based program. Other data are also provided according to the following tabular listings: Minor planet number, date of maximum elongation from the Sun in format yyyy/mm/dd, maximum elongation in degrees, right ascension on date of maximum elongation, declination on date of maximum elongation, both in J2000 coordinates, date of brightest magnitude in format yyyy/mm/dd, brightest magnitude, date of minimum distance in format yyyy/mm/dd, and minimum distance in AU.

Users should note that when the maximum elongation is about 177° or greater, the brightest magnitude is sharply peaked due to enhanced brightening near zero phase angle. Even as near as 10 days before or after minimum magnitude the magnitude is generally about 0.4 greater. This effect takes place in greater time interval for smaller maximum elongations. There is some interest in very small minimum phase angles. For maximum elongations E near 180° at Earth distance ∆, an approximate formula for the MINOR PLANETS AT UNUSUALLY FAVORABLE minimum phase angle is =(180°-E)/(∆+1). ELONGATIONS IN 2017 φ φ

Frederick Pilcher A special list of asteroids approaching the Earth more closely than 4438 Organ Mesa Loop 0.3 AU is provided following the list of temporal sequence of favorable elongations. Las Cruces, NM 88011 USA [email protected] CALL FOR FEEDBACK (Received: 2016 September 13) This is the 43rd consecutive year in which I have prepared for the A list is presented of minor planets that are much Minor Planet Bulletin a list of asteroids magnitude 14.5 and brighter than usual at their 2017 apparitions. A Call for brighter and becoming much brighter than usual at their coming Feedback is made regarding the ongoing utility of this apparitions. In the 1970’s and 1980’s most of the observing annual compilation, now in its 43rd consecutive year. activities of the Minor Planets Section were visual, and in many cases to a magnitude limit near 14. The lists were intended as recommendations for objects to observe visually. But now the The minor planets in the following lists will be much brighter at principal observing activities are with CCD cameras and to a their 2017 apparitions than at their average distances at maximum magnitude limit significantly fainter than 14.5. The quarterly elongation. Many years may pass before these planets will be reports, “Lightcurve Photometry Opportunities,” by Brian D. again as bright as in 2017. Observers are encouraged to give Warner, Alan W. Harris, Josef Durech, and Lance A. M. Benner special attention to those falling near the limit of their equipment. have become much better guides to objects for which current CCD observations of the types now being presented in these pages These lists have been prepared by an examination of the maximum would be especially valuable. This raises the question as to elongation circumstances of minor planets computed by the author whether this annual compilation should be continued into the for all years through 2060 with a full perturbation program written future, or whether this article should be the final installment. The by Dr. John Reed, and to whom he expresses his thanks. Elements author requests comments by readers as to the utility and rationale are from EMP 1992, except that for all planets for which new or for the continuation of this annual compilation. improved elements have been published subsequently in the Minor Planet Circulars or in electronic form, the newer elements have Editor’s Note: All interested readers are most kindly encouraged been used. Planetary positions are from the JPL DE-200 to make their responses either directly to Professor Pilcher ephemeris, courtesy of Dr. E. Myles Standish. and / or to the Editor .

Any planets whose brightest magnitudes near the time of Table I. Numerical Sequence of Favorable Elongations maximum elongation vary by at least 2.0 in this interval and in Planet Max Elon D Max E RA Dec Br Mag D Br Mag Min Dist D Min Dist

2017 will be within 0.3 of the brightest occurring, or vary by at 7 2017/10/30 171.8° 2h 4m +21° 2017/10/30 6.8 2017/10/30 0.849 least 3.0 and in 2017 will be within 0.5 of the brightest occurring; 10 2017/06/29 179.4° 18h35m -23° 2017/06/29 9.1 2017/06/27 1.845 14 2017/02/18 165.3° 10h31m +25° 2017/02/19 9.1 2017/02/23 1.236 and which are visual magnitude 14.5 or brighter, are included. For 20 2017/12/17 178.8° 5h41m +22° 2017/12/17 8.4 2017/12/19 1.093 25 2017/08/17 136.3° 20h25m +25° 2017/08/11 10.0 2017/08/09 0.927 planets brighter than visual magnitude 13.5, which are within the 31 2017/12/20 142.8° 6h16m +60° 2017/12/20 10.5 2017/12/20 1.601 range of a large number of observers, these standards have been 41 2017/03/08 174.7° 11h 6m + 0° 2017/03/09 9.6 2017/03/19 1.210 82 2017/02/09 175.3° 9h40m +18° 2017/02/09 10.6 2017/02/09 1.176 relaxed somewhat to include a larger number of planets. 89 2017/09/06 162.3° 22h43m +10° 2017/09/07 9.0 2017/09/07 1.103 105 2017/04/02 175.9° 12h57m - 1° 2017/04/03 10.5 2017/04/09 1.064 Magnitudes have been computed from the updated magnitude parameters published in MPC28104-28116, on 1996 Nov. 25, or 155 2017/11/01 179.0° 2h25m +13° 2017/11/01 13.5 2017/11/08 1.148 162 2017/01/10 170.5° 7h33m +31° 2017/01/11 12.3 2017/01/14 1.599 more recently in the Minor Planet Circulars. 166 2017/08/31 169.0° 23h 1m -18° 2017/09/02 12.6 2017/09/07 1.276 169 2017/08/12 173.8° 21h37m -20° 2017/08/12 11.5 2017/08/13 1.044 186 2017/10/07 179.6° 0h53m + 5° 2017/10/07 10.7 2017/10/02 1.081 Oppositions may be in right ascension or in celestial longitude. Here we use still a third representation, maximum elongation from Minor Planet Bulletin 44 (2017) 6

Planet Max Elon D Max E RA Dec Br Mag D Br Mag Min Dist D Min Dist Planet Max Elon D Max E RA Dec Br Mag D Br Mag Min Dist D Min Dist

211 2017/11/25 177.7° 4h 0m +22° 2017/11/25 11.1 2017/11/25 1.577 5604 2017/03/12 138.7° 8h54m -11° 2017/02/27 11.8 2017/02/24 0.034 249 2017/08/21 177.7° 22h 3m -14° 2017/08/21 12.9 2017/08/28 0.964 5851 2017/08/09 168.0° 20h57m - 4° 2017/08/08 14.5 2017/08/05 1.166 264 2017/10/05 169.2° 1h 1m - 5° 2017/10/06 11.5 2017/10/06 1.440 5913 2017/07/29 172.9° 20h38m -25° 2017/07/29 14.5 2017/08/04 1.214 270 2017/07/07 177.4° 19h 3m -20° 2017/07/07 10.3 2017/07/13 0.940 5964 2017/10/01 178.3° 0h31m + 1° 2017/10/01 14.1 2017/10/03 1.135 275 2017/02/21 177.3° 10h23m +12° 2017/02/21 11.5 2017/02/24 1.350 6053 2017/08/08 138.5° 23h28m + 8° 2017/08/23 14.1 2017/08/30 0.245

295 2017/12/13 178.8° 5h23m +24° 2017/12/13 12.8 2017/12/11 1.346 6063 2017/06/17 141.0° 15h38m + 1° 2017/05/31 13.0 2017/05/27 0.099 330 2017/09/25 169.8° 0h26m - 8° 2017/09/26 14.2 2017/10/01 0.908 6091 2017/08/27 179.0° 22h26m -10° 2017/08/27 14.1 2017/08/19 0.767 364 2017/10/19 167.8° 1h51m - 1° 2017/10/19 11.6 2017/10/22 0.942 6490 2017/07/28 161.0° 20h41m - 0° 2017/07/29 14.7 2017/07/30 0.589 365 2017/09/10 173.5° 23h 4m + 1° 2017/09/11 12.3 2017/09/14 1.498 6670 2017/07/18 174.5° 19h43m -15° 2017/07/19 13.7 2017/07/24 0.970 368 2017/06/29 169.9° 18h33m -13° 2017/06/30 13.3 2017/07/05 1.562 6914 2017/06/19 175.4° 17h50m -27° 2017/06/18 14.5 2017/06/14 0.965

376 2017/05/21 169.9° 15h42m -30° 2017/05/22 11.1 2017/05/25 0.902 7496 2017/12/23 178.3° 6h 6m +21° 2017/12/23 14.4 2017/12/13 1.232 415 2017/01/21 178.5° 8h11m +18° 2017/01/21 11.4 2017/01/11 1.186 7505 2017/10/20 166.1° 1h56m - 2° 2017/10/18 12.6 2017/10/14 0.653 435 2017/10/16 179.6° 1h26m + 9° 2017/10/16 12.1 2017/10/12 1.100 9671 2017/04/09 176.8° 13h 4m -10° 2017/04/09 13.7 2017/04/07 0.518 451 2017/12/11 176.0° 5h15m +18° 2017/12/11 10.4 2017/12/10 1.853 10487 2017/07/04 174.9° 19h 3m -27° 2017/07/04 14.5 2017/07/06 0.918 476 2017/07/01 177.8° 18h43m -25° 2017/07/01 11.4 2017/07/02 1.443 13538 2017/07/22 169.0° 20h24m -30° 2017/07/23 14.3 2017/07/24 0.712

492 2017/07/26 177.4° 20h25m -21° 2017/07/26 13.1 2017/07/30 1.634 20031 2017/07/31 173.2° 20h57m -23° 2017/07/31 14.5 2017/08/01 0.914 510 2017/06/25 162.9° 18h17m - 6° 2017/06/26 12.2 2017/06/28 1.140 21893 2017/08/15 173.2° 21h52m -20° 2017/08/15 14.4 2017/08/09 0.475 537 2017/08/07 175.4° 21h17m -20° 2017/08/07 11.6 2017/08/05 1.365 66146 2017/10/16 137.8° 3h 8m -24° 2017/10/23 12.2 2017/10/31 0.131 538 2017/09/13 174.8° 23h33m - 8° 2017/09/13 12.7 2017/09/14 1.640 138925 2017/08/02 171.0° 20h17m -13° 2017/08/02 13.7 2017/08/01 0.212 543 2017/12/07 171.3° 4h51m +31° 2017/12/07 12.9 2017/12/04 1.656 143404 2017/03/20 179.6° 11h57m - 0° 2017/04/12 13.2 2017/04/18 0.056

545 2017/08/12 175.4° 21h31m -19° 2017/08/12 12.3 2017/08/09 1.660 163696 2017/12/01 151.1° 5h37m +47° 2017/11/24 13.3 2017/11/21 0.094 554 2017/10/25 174.3° 1h50m +17° 2017/10/25 10.9 2017/10/27 1.056 171576 2017/10/31 140.7° 0h47m -17° 2017/10/23 12.6 2017/10/22 0.015 596 2017/05/30 179.3° 16h29m -21° 2017/05/30 11.7 2017/05/30 1.436 190166 2017/05/10 167.1° 15h42m - 7° 2017/07/15 14.2 2017/07/10 0.134 648 2017/01/01 177.1° 6h48m +25° 2017/01/01 12.9 2017/01/02 1.607 190166 2017/08/26 161.0° 21h14m - 0° 2017/07/15 14.2 2017/07/10 0.134 666 2017/11/15 175.5° 3h26m +14° 2017/11/14 12.7 2017/11/09 1.017

687 2017/10/13 158.2° 0h46m +28° 2017/10/13 13.9 2017/10/13 1.020 Table II. Temporal Sequence of Favorable Elongations 704 2017/10/01 152.4° 23h43m +28° 2017/10/01 9.9 2017/10/01 1.660 758 2017/10/26 171.6° 2h15m + 4° 2017/10/26 11.9 2017/10/28 1.764 763 2017/10/04 171.3° 0h25m +12° 2017/10/04 14.0 2017/10/03 0.875 Planet Max Elon D Max E RA Dec Br Mag D Br Mag Min Dist D Min Dist

804 2017/08/23 171.7° 22h17m -19° 2017/08/23 10.9 2017/08/22 1.437 648 2017/01/01 177.1° 6h48m +25° 2017/01/01 12.9 2017/01/02 1.607 898 2017/05/20 178.9° 15h45m -20° 2017/05/20 13.3 2017/06/05 0.880 5399 2017/01/05 178.4° 7h 2m +21° 2017/01/05 14.4 2017/01/03 1.320 905 2017/11/10 177.9° 2h58m +19° 2017/11/09 13.0 2017/11/05 0.911 162 2017/01/10 170.5° 7h33m +31° 2017/01/11 12.3 2017/01/14 1.599 913 2017/07/28 173.4° 20h40m -25° 2017/07/28 13.2 2017/07/24 0.829 4440 2017/01/17 166.5° 7h59m + 7° 2017/01/17 13.9 2017/01/19 0.817 415 2017/01/21 178.5° 8h11m +18° 2017/01/21 11.4 2017/01/11 1.186 916 2017/10/09 161.8° 0h38m +23° 2017/10/09 12.7 2017/10/06 0.829

955 2017/08/08 166.6° 21h22m -29° 2017/08/05 13.0 2017/07/28 0.942 2348 2017/01/23 171.8° 8h14m +11° 2017/01/23 14.3 2017/01/23 1.007

965 2017/12/30 148.2° 7h 8m +54° 2017/12/28 13.1 2017/12/27 1.380 1310 2017/02/06 143.5° 9h20m +52° 2017/01/26 13.0 2017/01/20 0.745 972 2017/11/12 168.8° 2h52m +28° 2017/11/11 12.6 2017/11/06 1.433 82 2017/02/09 175.3° 9h40m +18° 2017/02/09 10.6 2017/02/09 1.176 1252 2017/02/11 178.0° 9h42m +15° 2017/02/11 13.5 2017/02/17 1.353 983 2017/06/12 175.4° 17h27m -18° 2017/06/12 13.5 2017/06/11 1.874 988 2017/09/20 178.1° 23h53m - 2° 2017/09/20 14.0 2017/09/22 1.430 14 2017/02/18 165.3° 10h31m +25° 2017/02/19 9.1 2017/02/23 1.236 994 2017/09/26 179.4° 0h12m + 1° 2017/09/26 12.6 2017/09/24 1.245 275 2017/02/21 177.3° 10h23m +12° 2017/02/21 11.5 2017/02/24 1.350 1048 2017/06/10 166.4° 17h17m -36° 2017/06/09 12.5 2017/06/07 1.271 2546 2017/03/05 170.2° 10h53m - 3° 2017/03/06 14.3 2017/03/10 1.144 41 2017/03/08 174.7° 11h 6m + 0° 2017/03/09 9.6 2017/03/19 1.210 1072 2017/12/17 169.9° 5h37m +33° 2017/12/16 13.6 2017/12/13 1.460 5604 2017/03/12 138.7° 8h54m -11° 2017/02/27 11.8 2017/02/24 0.034 1116 2017/12/30 152.1° 6h44m +50° 2017/12/28 12.9 2017/12/27 1.357 1120 2017/09/06 179.2° 23h 2m - 6° 2017/09/06 14.1 2017/09/10 0.907 2577 2017/03/14 170.1° 11h12m - 5° 2017/03/13 14.3 2017/03/09 0.775 1132 2017/08/27 168.0° 22h38m -21° 2017/08/25 12.6 2017/08/18 1.014 143404 2017/03/20 179.6° 11h57m - 0° 2017/04/12 13.2 2017/04/18 0.056 105 2017/04/02 175.9° 12h57m - 1° 2017/04/03 10.5 2017/04/09 1.064 1134 2017/10/10 170.0° 0h59m +16° 2017/10/05 14.4 2017/09/20 0.504 1181 2017/12/11 179.7° 5h14m +23° 2017/12/11 13.6 2017/12/08 1.181 9671 2017/04/09 176.8° 13h 4m -10° 2017/04/09 13.7 2017/04/07 0.518 1227 2017/09/01 169.8° 22h56m -17° 2017/09/01 13.7 2017/08/28 1.675 190166 2017/05/10 167.1° 15h42m - 7° 2017/07/15 14.2 2017/07/10 0.134 1240 2017/09/15 171.3° 23h21m + 5° 2017/09/15 12.6 2017/09/13 1.369 898 2017/05/20 178.9° 15h45m -20° 2017/05/20 13.3 2017/06/05 0.880

1246 2017/07/30 169.0° 20h36m - 7° 2017/08/01 12.5 2017/08/08 0.880 376 2017/05/21 169.9° 15h42m -30° 2017/05/22 11.1 2017/05/25 0.902

1252 2017/02/11 178.0° 9h42m +15° 2017/02/11 13.5 2017/02/17 1.353 1319 2017/05/27 179.1° 16h15m -22° 2017/05/27 13.9 2017/05/23 1.423 1279 2017/07/06 170.2° 19h 3m -32° 2017/07/05 14.0 2017/07/03 0.865 596 2017/05/30 179.3° 16h29m -21° 2017/05/30 11.7 2017/05/30 1.436 1283 2017/10/12 170.2° 1h25m - 1° 2017/10/12 13.5 2017/10/12 1.503 1048 2017/06/10 166.4° 17h17m -36° 2017/06/09 12.5 2017/06/07 1.271 1299 2017/10/30 169.2° 2h32m + 3° 2017/10/30 14.2 2017/11/01 1.333 983 2017/06/12 175.4° 17h27m -18° 2017/06/12 13.5 2017/06/11 1.874

1310 2017/02/06 143.5° 9h20m +52° 2017/01/26 13.0 2017/01/20 0.745 1322 2017/06/12 170.9° 17h35m -14° 2017/06/12 14.2 2017/06/16 0.863 1319 2017/05/27 179.1° 16h15m -22° 2017/05/27 13.9 2017/05/23 1.423 5118 2017/06/12 176.3° 17h26m -19° 2017/06/13 14.3 2017/06/20 1.182 5066 2017/06/13 177.6° 17h33m -25° 2017/06/13 14.3 2017/06/14 0.623 1322 2017/06/12 170.9° 17h35m -14° 2017/06/12 14.2 2017/06/16 0.863 6063 2017/06/17 141.0° 15h38m + 1° 2017/05/31 13.0 2017/05/27 0.099 1326 2017/09/14 151.7° 0h26m -28° 2017/09/17 13.6 2017/09/19 1.165 3991 2017/06/19 177.8° 17h51m -25° 2017/06/19 14.5 2017/06/21 0.847 1358 2017/09/09 177.6° 23h14m - 7° 2017/09/09 14.3 2017/09/03 1.120 1362 2017/08/29 151.4° 23h43m -32° 2017/09/04 14.0 2017/09/09 1.215 6914 2017/06/19 175.4° 17h50m -27° 2017/06/18 14.5 2017/06/14 0.965 1369 2017/07/26 159.4° 19h58m + 0° 2017/07/26 14.1 2017/07/26 1.489 510 2017/06/25 162.9° 18h17m - 6° 2017/06/26 12.2 2017/06/28 1.140 1418 2017/08/27 174.1° 22h31m -15° 2017/08/27 13.2 2017/08/23 0.787 10 2017/06/29 179.4° 18h35m -23° 2017/06/29 9.1 2017/06/27 1.845 368 2017/06/29 169.9° 18h33m -13° 2017/06/30 13.3 2017/07/05 1.562 1608 2017/10/03 178.1° 0h33m + 5° 2017/10/03 14.4 2017/09/24 0.959 1619 2017/12/09 176.4° 5h 6m +26° 2017/12/09 13.7 2017/12/03 0.953 476 2017/07/01 177.8° 18h43m -25° 2017/07/01 11.4 2017/07/02 1.443

1719 2017/08/08 176.5° 21h16m -19° 2017/08/08 13.9 2017/08/16 1.295 10487 2017/07/04 174.9° 19h 3m -27° 2017/07/04 14.5 2017/07/06 0.918

1736 2017/10/22 172.6° 1h57m + 4° 2017/10/22 13.6 2017/10/23 0.874 2287 2017/07/05 177.9° 19h 0m -24° 2017/07/05 14.2 2017/07/09 0.866 1279 2017/07/06 170.2° 19h 3m -32° 2017/07/05 14.0 2017/07/03 0.865 1738 2017/07/29 168.7° 20h46m -29° 2017/07/29 13.4 2017/08/02 0.755 1883 2017/11/26 166.0° 4h 0m + 7° 2017/11/25 14.5 2017/11/22 0.818 270 2017/07/07 177.4° 19h 3m -20° 2017/07/07 10.3 2017/07/13 0.940 1982 2017/09/28 170.7° 0h30m - 6° 2017/09/26 13.8 2017/09/17 0.824 2728 2017/07/09 174.8° 19h10m -17° 2017/07/09 14.3 2017/07/10 1.041 2021 2017/09/15 176.3° 23h39m - 6° 2017/09/15 14.5 2017/09/08 0.849 3652 2017/07/11 176.7° 19h19m -18° 2017/07/11 14.4 2017/07/14 0.910 6670 2017/07/18 174.5° 19h43m -15° 2017/07/19 13.7 2017/07/24 0.970 2065 2017/11/03 168.2° 2h20m +26° 2017/11/03 14.4 2017/11/01 1.087 2152 2017/11/06 169.1° 2h29m +26° 2017/11/06 13.7 2017/11/04 1.463 13538 2017/07/22 169.0° 20h24m -30° 2017/07/23 14.3 2017/07/24 0.712 2228 2017/11/22 176.8° 3h53m +16° 2017/11/22 14.1 2017/11/22 1.576 492 2017/07/26 177.4° 20h25m -21° 2017/07/26 13.1 2017/07/30 1.634 2287 2017/07/05 177.9° 19h 0m -24° 2017/07/05 14.2 2017/07/09 0.866 1369 2017/07/26 159.4° 19h58m + 0° 2017/07/26 14.1 2017/07/26 1.489

913 2017/07/28 173.4° 20h40m -25° 2017/07/28 13.2 2017/07/24 0.829 2348 2017/01/23 171.8° 8h14m +11° 2017/01/23 14.3 2017/01/23 1.007 2440 2017/08/13 171.1° 21h19m - 6° 2017/08/12 14.5 2017/08/10 0.856 6490 2017/07/28 161.0° 20h41m - 0° 2017/07/29 14.7 2017/07/30 0.589 2546 2017/03/05 170.2° 10h53m - 3° 2017/03/06 14.3 2017/03/10 1.144 1738 2017/07/29 168.7° 20h46m -29° 2017/07/29 13.4 2017/08/02 0.755 2557 2017/10/03 179.5° 0h39m + 3° 2017/10/03 14.0 2017/10/03 0.985 5913 2017/07/29 172.9° 20h38m -25° 2017/07/29 14.5 2017/08/04 1.214 2577 2017/03/14 170.1° 11h12m - 5° 2017/03/13 14.3 2017/03/09 0.775 1246 2017/07/30 169.0° 20h36m - 7° 2017/08/01 12.5 2017/08/08 0.880

2585 2017/09/25 170.7° 0h26m - 7° 2017/09/26 14.0 2017/09/28 0.876 20031 2017/07/31 173.2° 20h57m -23° 2017/07/31 14.5 2017/08/01 0.914 2728 2017/07/09 174.8° 19h10m -17° 2017/07/09 14.3 2017/07/10 1.041 3699 2017/08/02 173.0° 21h 2m -24° 2017/08/03 14.4 2017/08/05 0.954 2731 2017/09/01 176.8° 22h48m -10° 2017/09/01 14.3 2017/08/26 1.767 138925 2017/08/02 171.0° 20h17m -13° 2017/08/02 13.7 2017/08/01 0.212 2860 2017/09/03 174.1° 22h45m - 1° 2017/09/04 14.5 2017/09/10 1.012 537 2017/08/07 175.4° 21h17m -20° 2017/08/07 11.6 2017/08/05 1.365 955 2017/08/08 166.6° 21h22m -29° 2017/08/05 13.0 2017/07/28 0.942 3122 2017/08/30 160.0° 21h17m -15° 2017/08/31 8.8 2017/09/01 0.047

3200 2017/12/10 158.2° 5h24m +44° 2017/12/14 10.7 2017/12/16 0.069 1719 2017/08/08 176.5° 21h16m -19° 2017/08/08 13.9 2017/08/16 1.295 3444 2017/11/20 166.9° 3h30m +32° 2017/11/20 14.1 2017/11/21 0.908 4460 2017/08/08 170.1° 21h19m -25° 2017/08/09 14.2 2017/08/12 1.487 3652 2017/07/11 176.7° 19h19m -18° 2017/07/11 14.4 2017/07/14 0.910 6053 2017/08/08 138.5° 23h28m + 8° 2017/08/23 14.1 2017/08/30 0.245 5851 2017/08/09 168.0° 20h57m - 4° 2017/08/08 14.5 2017/08/05 1.166 3699 2017/08/02 173.0° 21h 2m -24° 2017/08/03 14.4 2017/08/05 0.954 3702 2017/09/24 152.8° 0h57m -23° 2017/09/25 14.0 2017/09/25 1.057 169 2017/08/12 173.8° 21h37m -20° 2017/08/12 11.5 2017/08/13 1.044

3744 2017/10/10 176.1° 0h57m +10° 2017/10/10 14.5 2017/10/17 0.982 545 2017/08/12 175.4° 21h31m -19° 2017/08/12 12.3 2017/08/09 1.660 3991 2017/06/19 177.8° 17h51m -25° 2017/06/19 14.5 2017/06/21 0.847 2440 2017/08/13 171.1° 21h19m - 6° 2017/08/12 14.5 2017/08/10 0.856 21893 2017/08/15 173.2° 21h52m -20° 2017/08/15 14.4 2017/08/09 0.475 4440 2017/01/17 166.5° 7h59m + 7° 2017/01/17 13.9 2017/01/19 0.817 4460 2017/08/08 170.1° 21h19m -25° 2017/08/09 14.2 2017/08/12 1.487 25 2017/08/17 136.3° 20h25m +25° 2017/08/11 10.0 2017/08/09 0.927 4614 2017/08/23 174.4° 21h59m - 6° 2017/08/23 14.3 2017/08/20 0.765 249 2017/08/21 177.7° 22h 3m -14° 2017/08/21 12.9 2017/08/28 0.964

5066 2017/06/13 177.6° 17h33m -25° 2017/06/13 14.3 2017/06/14 0.623 804 2017/08/23 171.7° 22h17m -19° 2017/08/23 10.9 2017/08/22 1.437 4614 2017/08/23 174.4° 21h59m - 6° 2017/08/23 14.3 2017/08/20 0.765 5118 2017/06/12 176.3° 17h26m -19° 2017/06/13 14.3 2017/06/20 1.182 190166 2017/08/26 161.0° 21h14m - 0° 2017/07/15 14.2 2017/07/10 0.134 5133 2017/12/04 174.2° 4h42m +16° 2017/12/03 14.3 2017/11/25 1.349 5189 2017/10/21 148.7° 0h38m -16° 2017/10/01 13.7 2017/09/26 0.061 1132 2017/08/27 168.0° 22h38m -21° 2017/08/25 12.6 2017/08/18 1.014 5399 2017/01/05 178.4° 7h 2m +21° 2017/01/05 14.4 2017/01/03 1.320 1418 2017/08/27 174.1° 22h31m -15° 2017/08/27 13.2 2017/08/23 0.787 Minor Planet Bulletin 44 (2017) 7

Planet Max Elon D Max E RA Dec Br Mag D Br Mag Min Dist D Min Dist LIGHTCURVES FROM THE ARCHIVE: 6091 2017/08/27 179.0° 22h26m -10° 2017/08/27 14.1 2017/08/19 0.767 1362 2017/08/29 151.4° 23h43m -32° 2017/09/04 14.0 2017/09/09 1.215 1090 SUMIDA, 2284 SAN JUAN, AND 3493 STEPANOV 3122 2017/08/30 160.0° 21h17m -15° 2017/08/31 8.8 2017/09/01 0.047 166 2017/08/31 169.0° 23h 1m -18° 2017/09/02 12.6 2017/09/07 1.276 1227 2017/09/01 169.8° 22h56m -17° 2017/09/01 13.7 2017/08/28 1.675 Kim Lang

2731 2017/09/01 176.8° 22h48m -10° 2017/09/01 14.3 2017/08/26 1.767 Klokkerholm Observatory 2860 2017/09/03 174.1° 22h45m - 1° 2017/09/04 14.5 2017/09/10 1.012 89 2017/09/06 162.3° 22h43m +10° 2017/09/07 9.0 2017/09/07 1.103 Blomstervaenget 15, DK-9320 Klokkerholm 1120 2017/09/06 179.2° 23h 2m - 6° 2017/09/06 14.1 2017/09/10 0.907 [email protected] 1358 2017/09/09 177.6° 23h14m - 7° 2017/09/09 14.3 2017/09/03 1.120

365 2017/09/10 173.5° 23h 4m + 1° 2017/09/11 12.3 2017/09/14 1.498 538 2017/09/13 174.8° 23h33m - 8° 2017/09/13 12.7 2017/09/14 1.640 (Received: 2016 October 15) 1326 2017/09/14 151.7° 0h26m -28° 2017/09/17 13.6 2017/09/19 1.165 1240 2017/09/15 171.3° 23h21m + 5° 2017/09/15 12.6 2017/09/13 1.369 2021 2017/09/15 176.3° 23h39m - 6° 2017/09/15 14.5 2017/09/08 0.849 Three asteroids were observed briefly between other

988 2017/09/20 178.1° 23h53m - 2° 2017/09/20 14.0 2017/09/22 1.430 projects in 2015 March and April. The lightcurves of 3702 2017/09/24 152.8° 0h57m -23° 2017/09/25 14.0 2017/09/25 1.057 330 2017/09/25 169.8° 0h26m - 8° 2017/09/26 14.2 2017/10/01 0.908 1090 Sumida and 3493 Stepanov shows amplitudes of 2585 2017/09/25 170.7° 0h26m - 7° 2017/09/26 14.0 2017/09/28 0.876 994 2017/09/26 179.4° 0h12m + 1° 2017/09/26 12.6 2017/09/24 1.245 A = 0.30 and A = 0.95 mag. For 2284 San Juan, a

1982 2017/09/28 170.7° 0h30m - 6° 2017/09/26 13.8 2017/09/17 0.824 synodic period of P = 9.18 h and amplitude of A = 0.69 704 2017/10/01 152.4° 23h43m +28° 2017/10/01 9.9 2017/10/01 1.660 mag were found. 5964 2017/10/01 178.3° 0h31m + 1° 2017/10/01 14.1 2017/10/03 1.135 1608 2017/10/03 178.1° 0h33m + 5° 2017/10/03 14.4 2017/09/24 0.959 2557 2017/10/03 179.5° 0h39m + 3° 2017/10/03 14.0 2017/10/03 0.985

763 2017/10/04 171.3° 0h25m +12° 2017/10/04 14.0 2017/10/03 0.875 Photometric observations of three asteroids were carried out with a 264 2017/10/05 169.2° 1h 1m - 5° 2017/10/06 11.5 2017/10/06 1.440 186 2017/10/07 179.6° 0h53m + 5° 2017/10/07 10.7 2017/10/02 1.081 0.20-m Newtonian telescope fitted with a coma corrector giving 916 2017/10/09 161.8° 0h38m +23° 2017/10/09 12.7 2017/10/06 0.829 1134 2017/10/10 170.0° 0h59m +16° 2017/10/05 14.4 2017/09/20 0.504 an effective focal length of 890 mm. The camera was an Atik

3744 2017/10/10 176.1° 0h57m +10° 2017/10/10 14.5 2017/10/17 0.982 383L+ with a Kodak KAF-8300 CCD chip and pixel size of 1283 2017/10/12 170.2° 1h25m - 1° 2017/10/12 13.5 2017/10/12 1.503 687 2017/10/13 158.2° 0h46m +28° 2017/10/13 13.9 2017/10/13 1.020 5.4x5.4 µm. All images were unbinned and taken through a clear 435 2017/10/16 179.6° 1h26m + 9° 2017/10/16 12.1 2017/10/12 1.100 66146 2017/10/16 137.8° 3h 8m -24° 2017/10/23 12.2 2017/10/31 0.131 filter. For timekeeping software Dimension 4 (Thinking Man Software) was used. Master darks and flats were used to calibrate 364 2017/10/19 167.8° 1h51m - 1° 2017/10/19 11.6 2017/10/22 0.942 7505 2017/10/20 166.1° 1h56m - 2° 2017/10/18 12.6 2017/10/14 0.653 the raw science frames using IRIS 5.59 software (Buil, 2011). A 5189 2017/10/21 148.7° 0h38m -16° 2017/10/01 13.7 2017/09/26 0.061 1736 2017/10/22 172.6° 1h57m + 4° 2017/10/22 13.6 2017/10/23 0.874 search of the asteroid lightcurve database (LCDB; Warner et al. 554 2017/10/25 174.3° 1h50m +17° 2017/10/25 10.9 2017/10/27 1.056 2009) as of 2016 July was done for each of the observed asteroids. 758 2017/10/26 171.6° 2h15m + 4° 2017/10/26 11.9 2017/10/28 1.764 7 2017/10/30 171.8° 2h 4m +21° 2017/10/30 6.8 2017/10/30 0.849 All three asteroids were listed in the MPB photometry 1299 2017/10/30 169.2° 2h32m + 3° 2017/10/30 14.2 2017/11/01 1.333 opportunities list for 2015 January-March (Warner et al., 2015). 171576 2017/10/31 140.7° 0h47m -17° 2017/10/23 12.6 2017/10/22 0.015 155 2017/11/01 179.0° 2h25m +13° 2017/11/01 13.5 2017/11/08 1.148

2065 2017/11/03 168.2° 2h20m +26° 2017/11/03 14.4 2017/11/01 1.087 The calibrated images were analyzed using MPO Canopus 2152 2017/11/06 169.1° 2h29m +26° 2017/11/06 13.7 2017/11/04 1.463 905 2017/11/10 177.9° 2h58m +19° 2017/11/09 13.0 2017/11/05 0.911 10.7.1.3 (Warner, 2011). The Comp Star Selector utility of MPO 972 2017/11/12 168.8° 2h52m +28° 2017/11/11 12.6 2017/11/06 1.433 666 2017/11/15 175.5° 3h26m +14° 2017/11/14 12.7 2017/11/09 1.017 Canopus was used to select up to five comparison stars of near solar-color for the differential photometry. Equal size apertures for 2329 2017/11/20 115.9° 2h 5m -40° 2017/10/08 14.1 2017/09/30 0.158 3444 2017/11/20 166.9° 3h30m +32° 2017/11/20 14.1 2017/11/21 0.908 target and comparison stars where used to minimize the effects of 2228 2017/11/22 176.8° 3h53m +16° 2017/11/22 14.1 2017/11/22 1.576 211 2017/11/25 177.7° 4h 0m +22° 2017/11/25 11.1 2017/11/25 1.577 changing seeing conditions. 1883 2017/11/26 166.0° 4h 0m + 7° 2017/11/25 14.5 2017/11/22 0.818

163696 2017/12/01 151.1° 5h37m +47° 2017/11/24 13.3 2017/11/21 0.094 5133 2017/12/04 174.2° 4h42m +16° 2017/12/03 14.3 2017/11/25 1.349 1090 Sumida was in opposition on 2015 March 25 and observed 543 2017/12/07 171.3° 4h51m +31° 2017/12/07 12.9 2017/12/04 1.656 on March 10. The LCDB gives a period of P =2.719 h (Behrend, 1619 2017/12/09 176.4° 5h 6m +26° 2017/12/09 13.7 2017/12/03 0.953 3200 2017/12/10 158.2° 5h24m +44° 2017/12/14 10.7 2017/12/16 0.069 2015) with a quality code of U = 3. The phased plot using the

451 2017/12/11 176.0° 5h15m +18° 2017/12/11 10.4 2017/12/10 1.853 latest data has been forced to this period. 1181 2017/12/11 179.7° 5h14m +23° 2017/12/11 13.6 2017/12/08 1.181 295 2017/12/13 178.8° 5h23m +24° 2017/12/13 12.8 2017/12/11 1.346 20 2017/12/17 178.8° 5h41m +22° 2017/12/17 8.4 2017/12/19 1.093 1072 2017/12/17 169.9° 5h37m +33° 2017/12/16 13.6 2017/12/13 1.460

31 2017/12/20 142.8° 6h16m +60° 2017/12/20 10.5 2017/12/20 1.601 7496 2017/12/23 178.3° 6h 6m +21° 2017/12/23 14.4 2017/12/13 1.232 965 2017/12/30 148.2° 7h 8m +54° 2017/12/28 13.1 2017/12/27 1.380 1116 2017/12/30 152.1° 6h44m +50° 2017/12/28 12.9 2017/12/27 1.357

Table III. Temporal list of approaches closer than 0.3 AU

5604 2017/03/12 138.7° 8h54m -11° 2017/02/27 11.8 2017/02/24 0.034 143404 2017/03/20 179.6° 11h57m - 0° 2017/04/12 13.2 2017/04/18 0.056 6063 2017/06/17 141.0° 15h38m + 1° 2017/05/31 13.0 2017/05/27 0.099 138925 2017/08/02 171.0° 20h17m -13° 2017/08/02 13.7 2017/08/01 0.212 6053 2017/08/08 138.5° 23h28m + 8° 2017/08/23 14.1 2017/08/30 0.245

190166 2017/08/26 161.0° 21h14m - 0° 2017/07/15 14.2 2017/07/10 0.134 3122 2017/08/30 160.0° 21h17m -15° 2017/08/31 8.8 2017/09/01 0.047 66146 2017/10/16 137.8° 3h 8m -24° 2017/10/23 12.2 2017/10/31 0.131 171576 2017/10/31 140.7° 0h47m -17° 2017/10/23 12.6 2017/10/22 0.015 2329 2017/11/20 115.9° 2h 5m -40° 2017/10/08 14.1 2017/09/30 0.158

163696 2017/12/01 151.1° 5h37m +47° 2017/11/24 13.3 2017/11/21 0.094 3200 2017/12/10 158.2° 5h24m +44° 2017/12/14 10.7 2017/12/16 0.069

The lightcurve is somewhat sparse in sampling so a Fourier fit is omitted. An ensemble of four comparison stars was used; the standard deviation of the ensemble was ± 0.030 mag.

Minor Planet Bulletin 44 (2017) 8

2284 San Juan was observed on two nights: 2015 March 10 and April 3. Exposure times were 300 s in sessions 74 and 76 and 120 s in session 75. The phased plot supports the period of P = 9.18 h found by Brinsfield (2008). The period of 9.16 h given in the LCDB for this paper appears to be a misprint. Due to the long interval between the observations, there were a number of alias periods in the period spectrum separated by approximately 0.09 h.

The lightcurve is marginally complete, so a Fourier fit is omitted. An ensemble of five solar-like comparison stars was used; the standard deviation of ensemble was ± 0.014 mag.

References

Behrend, R. (2015). Observatoire de Geneve website. http://obswww.unige.ch/~behrend/page_cou.html The legend in the lightcurve is somewhat misleading. Brinsfield, J.W. (2008). “Asteroid Lightcurve Analysis at the Via Observations on the night of March 13 began with exposure times Capote Observatory: First Quarter 2008.” Minor Planet Bull. 35, of 300 s. After the meridian flip, the exposure time was set by 119-122. mistake to 120 s. These data appear as session 76. An hour went by before the error was discovered and reset to 300 s. All Buil, C. (2011). IRIS v5.59 observations of 300 s are in session 75. Most of the observations http://www.astrosurf.com/buil/us/iris/iris.htm in session 76 were done after midnight and so labeled March 14. Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). Session 75 and 76 are actually from the same night. “Lightcurves and phase relations of the asteroids 82 Alkmene and 3493 Stepanov was in opposition on 2015 March 7 and observed 444 Gyptis.” Icarus 57, 251-258. on March 12. The LCDB gives periods of 6.112 h (Stephens, Moravec, P., Letfullina, A., Ditteon, R. (2013). “Asteroid 2012) and 6.12 h (Moravec et al., 2013). The phased plot using the Lightcurve Analysis at the Oakley Observatories: 2012 May – latest data has been forced to the period found by Stephens. June.” Minor Planet Bull. 40, 17-20.

Stephens, R.D. (2012). “Asteroids Observed from Santana, CS3 and GMARS Observatories: 2012 April – June.” Minor Planet Bull. 39-4, 226-228.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid lightcurve database.” Icarus 202, 134-146. Updated 2016 July. http://www.MinorPlanet.info/lightcurvedatabase.html

Warner, B.D. (2013). Bdw Publishing MPO Software. MPO Canopus v10.4.3.21

Warner, B.D., Harris, A.W., Durech, J., Benner, L.A.M. (2015). “Lightcurve photometry opportunities: 2015 January-March.” Minor Planet Bull. 42, 83-86.

Number Name 2015 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. Grp 1090 Sumida 03/10 33 8.8 160 9 2.719 0.001 0.25 0.02 PHO 2284 San Juan 03/13-04/03 137 3.7,14.1 166 3 9.1814 0.0004 0.62 0.03 FLOR 3493 Stepanov 03/12 67 4.9 166 6 6.112 0.001 0.95 0.03 FLOR

Table I. Observing circumstances and results. Pts is the number of data points used in the analysis. The phase angle values are for the first and last date, unless a minimum (second value) was reached. LPAB and BPAB are the average phase angle bisector longitude and latitude. Period is in hours. Amp is peak-to-peak amplitude. LPAB and BPAB are the average phase angle bisector longitude and latitude (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009). Minor Planet Bulletin 44 (2017) 9

ROTATION PERIOD DETERMINATIONS FOR Kryszczynska, A., and 29 coauthors (2012). “Do Slivan states 392 WILHELMINA AND 864 AASE exist in the Flora family?. I. Photometric survey of the Flora Region.” Astron. Astrophys. 546, A72. Frederick Pilcher 4438 Organ Mesa Loop Las Cruces, NM 88011 USA [email protected]

(Received: 2016 September 21)

Synodic rotation periods and amplitudes are found for 392 Wilhelmina 13.058 ± 0.001 hours, 0.10 ± 0.01 magnitudes; and 864 Aase 3.2324 ± 0.0001 hours, 0.38 ± 0.03 magnitudes.

Observations to produce period determinations for 392 Wilhelmina and 864 Aase were made at the Organ Mesa Observatory with a 35.4 cm Meade LX200 GPS S-C and SBIG STL 1001-E CCD, 60 second exposure times, unguided, clear filter. Photometric measurement and lightcurve construction are with MPO Canopus software. To reduce the number of points on the lightcurves and make them easier to read data points have been binned in sets of 3 with maximum time difference 5 minutes.

392 Wilhelmina. Previous rotation period determinations have been made by Harris et al. (1999), 8.54 h; Behrend (2001), 8.54 h; Gil-Hutton and Canada (2003), 17.961 h; and Garceran et al. (2016), 16.98 h. New observations on 6 nights 2016 Aug. 17 – Sept. 20 provide a good fit to an irregular lightcurve with period 13.058 ± 0.001 hours, amplitude 0.10 ± 0.01 magnitudes. This rotation period disagrees with all previous published periods. A good fit can also be found to a trial double period of 26.119 hours, for which the two sides of the lightcurve are almost identical to each other and to the 13.058 hour lightcurve. The 26.119 hour lightcurve would require an asteroid with an irregular shape and also be symmetrical about a 180 degree rotation. The probability for a real asteroid to have such high symmetry is negligible and the double period can be safely rejected. A period spectrum between 8 hours and 20 hours is also presented. Trial lightcurves plotted to all the minima in the period spectrum except 13.058 hours showed large misfits among the several sessions. The 13.058 hour period can be considered secure.

864 Aase. The only previously published period is 3.2329 hours by Kryszczynska et al. (2012). New observations on 5 nights 2016 June 18 – July 10 provide a good fit to an almost symmetrical bimodal lightcurve with period 3.2324 ± 0.0001 hours and amplitude 0.38 ± 0.03 magnitudes. This is in excellent agreement with Kryszczynska et al.

References

Behrend, R. (2001). Observatoire de Geneve web site, http://obswww.unige.ch/~behrend/page_cou.html.

Garceran, A.C., Aznar, A., Mansego, E.A., Rodriguez, P.B., de Haro, J.L., Fornas Silva, A., Fornas Silva, G., Martinez, V.M., Chiner, O.R. (2016). “Nineteen Asteroids Lightcurves at Asteroids Observers (OBAS) - MPPD: 2015 April-September.” Minor Planet Bull. 43, 92-97

Gil-Hutton, R., and Canada, M. (2003). “Photometry of fourteen Main Belt Asteroids.” Rev. Mexicana Astron. Astrof. 39, 69-76.

Harris, A.W., Young, J.W., Bowell, E., Tholen, D.J. (1999). “Asteroid Lightcurve Observations from 1981 to 1983.” Icarus 142, 173-201. Minor Planet Bulletin 44 (2017) 10 ASTEROID-DEEPSKY APPULSES IN 2017 The table gives the following data:

Brian D. Warner Date/Time Universal Date (MM DD) and Time of closest Center for Solar System Studies approach 446 Sycamore Ave. #/Asteroid The number and name of the asteroid Eaton, CO 80615 RA/Dec The J2000 position of the asteroid [email protected] AM The approximate visual magnitude of the asteroid (Received: 2016 September 29) Sep/PA The separation in arcseconds and the position angle from the DSO to the asteroid The following list is a very small subset of the results of a search DSO The DSO name or catalog designation for asteroid-deepsky appulses for 2017, presenting only the highlights for the year based on close approaches of brighter DM The approximate total magnitude of the DSO asteroids to brighter DSOs. The complete set of predictions is DT The type of DSO: OC = Open Cluster; GC = available at Globular Cluster; G = Galaxy http://www.minorplanet.info/ObsGuides/Appulses/DSOAppulses.htm SE/ME The elongation in degrees from the sun and moon respectively For any event not covered, the Minor Planet Center's web site at http://www.minorplanetcenter.net/cgi-bin/checkmp.cgi allows you MP The phase of the moon: 0 = New, 1.0 = Full. to enter the location of a suspected asteroid or supernova and Positive = waxing; Negative = waning check if there are any known targets in the area.

Date UT # Name RA Dec AM Sep PA DSO DM DT SE ME MP ------01 05 18 57 760 Massinga 07 36.90 +35 16.2 11.8 70 360 NGC 2415 12.4 G 166 96 0.50 01 20 08 11 18 Melpomene 02 38.26 +02 07.8 10.0 59 328 NGC 1016 11.6 G 97 171 -0.46 01 24 06 39 785 Zwetana 09 48.74 +33 26.6 12.6 142 46 NGC 3003 11.9 G 157 120 -0.13 01 26 04 03 234 Barbara 03 06.90 +00 47.1 13.4 6 140 NGC 1211 12.3 G 98 119 -0.03 02 01 07 32 266 Aline 08 56.10 -03 21.1 13.1 6 192 NGC 2708 12.0 G 160 128 0.20 02 03 16 26 618 Elfriede 11 13.52 +22 10.2 13.6 20 53 UGC 6253 12.0 G 150 122 0.45 02 21 05 41 348 May 12 27.86 +12 15.8 13.9 177 222 NGC 4440 11.7 G 148 87 -0.28 02 23 07 36 519 Sylvania 09 52.17 +29 18.4 14.0 271 11 NGC 3032 12.5 G 159 149 -0.12 02 23 09 32 70 Panopaea 12 27.92 +12 16.0 12.5 138 210 NGC 4440 11.7 G 150 113 -0.11 02 24 02 24 348 May 12 26.47 +12 34.6 13.8 184 219 NGC 4413 12.3 G 151 122 -0.07 02 25 04 17 348 May 12 25.89 +12 41.7 13.8 134 38 NGC 4388 11.0 G 152 136 -0.02 02 25 17 52 348 May 12 25.59 +12 45.5 13.8 279 221 NGC 4387 12.1 G 153 143 -0.01 02 26 18 53 348 May 12 25.01 +12 52.4 13.8 126 219 M84 9.1 G 154 156 0.00 03 03 04 08 269 Justitia 10 55.46 +07 46.2 13.2 288 29 NGC 3462 12.2 G 179 120 0.25 03 04 05 46 369 Aeria 12 00.64 +20 05.9 12.8 65 33 NGC 4032 12.3 G 160 115 0.36 03 21 23 38 250 Bettina 14 47.71 -19 01.0 12.8 249 342 NGC 5757 11.9 G 136 61 -0.37 03 22 01 05 247 Eukrate 13 18.90 -21 03.2 13.0 11 172 NGC 5068 10.0 G 153 82 -0.37 03 22 18 20 105 Artemis 13 04.35 -05 32.0 10.9 147 67 NGC 4941 11.1 G 165 99 -0.30 03 23 21 48 782 Montefiore 12 55.94 +04 19.5 13.6 96 22 NGC 4808 11.7 G 168 118 -0.20 04 02 01 09 720 Bohlinia 13 04.30 -05 28.6 13.4 279 19 NGC 4941 11.1 G 175 117 0.31 04 28 02 06 112 Iphigenia 13 20.34 -12 33.5 13.4 99 22 NGC 5088 12.4 G 165 142 0.04 04 28 16 03 41 Daphne 10 52.14 +10 08.5 10.6 45 134 NGC 3433 11.6 G 122 92 0.07 05 02 06 41 230 Athamantis 12 59.27 -15 02.4 10.9 37 225 NGC 4856 10.5 G 156 78 0.41 06 18 06 28 107 Camilla 23 36.55 +00 15.8 13.6 139 162 NGC 7716 12.1 G 92 14 -0.41 06 20 20 02 691 Lehigh 18 04.77 -24 18.5 13.6 91 344 NGC 6530 4.6 OC 178 132 -0.15 06 21 09 26 346 Hermentaria 18 02.32 -23 03.3 10.9 82 168 M20 6.3 CNB 179 141 -0.11 06 22 15 00 691 Lehigh 18 03.14 -24 24.7 13.5 106 164 M8 5.0 CNB 179 159 -0.03 07 17 17 00 30 Urania 14 24.28 -16 45.3 12.4 78 192 NGC 5595 12.0 G 104 172 -0.40 07 18 03 37 30 Urania 14 24.51 -16 45.9 12.4 66 10 NGC 5597 12.0 G 104 172 -0.35 07 20 00 38 324 Bamberga 17 40.75 -36 58.0 10.5 68 211 NGC 6400 8.8 OC 146 156 -0.16 07 22 20 07 1248 Jugurtha 22 00.31 -24 35.2 14.0 228 318 NGC 7167 12.5 G 154 146 0.00 08 17 23 53 89 Julia 23 04.45 +08 55.7 9.3 258 31 NGC 7469 12.3 G 151 104 -0.18 09 16 21 34 270 Anahita 18 54.61 -19 54.1 12.0 68 176 NGC 6716 7.5 OC 109 151 -0.13 09 22 08 43 271 Penthesilea 22 55.65 -05 27.8 13.7 139 343 NGC 7416 12.4 G 164 138 0.05 09 24 16 06 435 Ella 01 44.86 +10 22.4 12.8 220 165 NGC 665 12.1 G 154 154 0.20 10 14 06 12 8 Flora 06 55.01 +18 04.0 9.9 179 4 NGC 2304 10.0 OC 98 31 -0.31 10 17 07 48 66146 1998 TU3 03 04.12 -26 02.0 12.3 86 314 NGC 1201 10.7 G 138 128 -0.06 10 17 22 07 337 Devosa 23 36.50 +00 18.6 12.0 38 354 NGC 7716 12.1 G 150 170 -0.04 11 19 09 01 364 Isara 01 27.76 -01 53.8 12.3 58 215 NGC 564 12.5 G 141 133 0.01 11 20 23 05 628 Christine 02 30.62 -02 52.1 13.1 174 6 NGC 958 12.1 G 151 128 0.06 11 26 15 02 364 Isara 01 25.81 -01 21.1 12.5 186 249 NGC 545 12.2 G 134 46 0.49 11 26 15 40 364 Isara 01 25.80 -01 21.0 12.5 3 67 NGC 541 12.1 G 134 46 0.50 12 11 08 25 631 Philippina 07 09.37 +00 47.4 12.8 49 321 NGC 2346 12.5 PN 143 76 -0.39 12 11 19 37 17 Thetis 05 12.10 +16 41.3 11.5 44 180 NGC 1817 7.7 OC 174 110 -0.34 12 12 16 32 625 Xenia 05 35.15 +10 00.6 13.9 281 9 Cr 69 2.8 OC 166 116 -0.26 12 16 12 32 796 Sarita 07 10.83 +50 07.5 12.7 178 213 NGC 2340 11.7 G 147 132 -0.03 12 20 04 43 796 Sarita 07 05.59 +50 35.8 12.7 15 204 NGC 2320 11.9 G 149 149 0.03 12 21 23 35 597 Bandusia 06 15.16 +39 48.8 13.1 136 191 NGC 2192 10.9 OC 163 139 0.12

Minor Planet Bulletin 44 (2017) 11

LIGHTCURVE AND ROTATION PERIOD FOR MINOR PLANET 1715 SALLI

Mike Foylan Cherryvalley Observatory, I83, Cherryvalley, Rathmolyon, Co. Meath, Ireland [email protected]

(Received: 2016 October 3)

CCD photometric observations in Bessell I-band of minor planet 1715 Salli (1938 GK) were made in 2016 March and April. A synodic rotation period of 11.0815 ± 0.0117 h and amplitude of A = 0.61 ± 0.05 mag were determined from the eight nights of observations.

The main-belt asteroid 1715 Salli was discovered 1938 April 9 by H. Alikoski at Turku in Finland and is named in honour of the Acknowledgements wife of the discoverer. Its orbital period is approximately 3.71 years. The absolute magnitude H = 12.2 and assumed albedo of The author wishes to express gratitude to Alessandro Marchini, 0.044 (JPL, 2016) give an estimated diameter of 24 km. Bus and Astronomical Observatory, DSFTA - University of Siena (K54), Binzel (2002) observed 1715 Salli during Phase II of the Small Riccardo Papini Carpione Observatory (K49) and Fabio Main Belt Asteroid Spectrographic Survey (SMASS II) and Salvaggio, Saronno observatory for their dedication and work on assigned a taxonomic classification of X-type, described generally minor planets and variable stars. as a featureless spectrum with slight to moderately reddish slope. References Cherryvalley Observatory (MPC Code I83) is an amateur observatory located in eastern rural Ireland. Observations with an Bus, S.J., Binzel, R.P. (2002). “Phase II of the Small Main-Belt I-band Bessel photometric filter were conducted with a 0.2-m Asteroid Spectroscopic Survey.” Icarus 158, 106–145. Schmidt-Cassegrain Telescope (SCT) operating at f/7.6 using an SBIG STL-1301E CCD camera with a 1280x1024 array of 16- Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., micron pixels. The resulting image scale was 2.15 arcsecond per Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, pixel. Image acquisition was undertaken with Software Bisque’s H., Zeigler, K.W. (1989). “Photoelectric Observations of TheSky6 Professional and CCDSoft v5. All light images were Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. aligned, dark and flat-field corrected using CCDSoft v5 with mid- exposure times light-time corrected using MPO Canopus JPL (2016). Small-Body Database Browser - JPL Solar System v10.4.3.17. A total of 604 data points were used in the Dynamics web site. http://ssd.jpl.nasa.gov/sbdb.cgi calculations. Table I gives the observing circumstances and results. Mansego, E.A., Rodriguez, P.B., de Haro, J.L., Chiner, O.R., Silva, A.F., Porta, D.H. Martinez, V.M., Silva, G.F. Garceran, Data were reduced in MPO Canopus using differential photometry A.C. (2016). “Eighteen asteroids lightcurves at Asteroides to facilitate easy exportation. Night-to-night zero point calibration Observers (OBAS) - MPPD: 2016 March - May.” Minor Planet was accomplished by selecting up to five comparison stars with Bulletin 43, 332-336. near solar colours using the “comp star selector” (CSS) feature. Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid The Cousins I Magnitudes for the comparisons were derived using the 2MASS to BVRI formulae developed by Warner (2007). Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sept. http://www.MinorPlanet.info/lightcurvedatabase.html Period analysis was completed using MPO Canopus, which incorporates the Fourier analysis algorithm (FALC) developed by Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., Harris (Harris et al. 1989). Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., The phased plot of the data demonstrates a classical bimodal Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light shape. The period solution of 11.0815 ± 0.0117 h is in close Curves from the Palomar Transient Factory Survey: Rotation agreement with recently published work by a Spanish based group Periods and Phase Functions from Sparse Photometry.” Astron. J. 150, A75. of astronomers (OBAS; Mansego et al., 2016) who found a period of 11.087 ± 0.001 h. Earlier work by Waszczak et al. (2015) found Warner, B.D. (2007). “Initial Results of a Dedicated H-G a period 11.1667 h and amplitude of 0.22 mag. Program.” Minor Planet Bul. 34, 113-119.

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. Group 1715 Salli 03/30-04/27 604 6.8,19.1 186 8 11.0815 0.0117 0.61 0.03 MBA

Table I. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude.

Minor Planet Bulletin 44 (2017) 12

ASTEROID LIGHTCURVE ANALYSIS AT adopted amplitude for the lightcurve. The value is meant only to CS3-PALMER DIVIDE STATION: be a quick guide. 2016 JULY-SEPTEMBER For the sake of brevity, only some of the previously reported Brian D. Warner results may be referenced in the discussions on specific asteroids. Center for Solar System Studies – Palmer Divide Station For a more complete listing, the reader is directed to the asteroid 446 Sycamore Ave. lightcurve database (LCDB; Warner et al., 2009a). The on-line Eaton, CO 80615 USA version at http://www.minorplanet.info/lightcurvedatabase.html [email protected] allows direct queries that can be filtered a number of ways and the results saved to a text file. A set of text files of the main LCDB (Received: 2016 October 3) tables, including the references with bibcodes, is also available for download. Readers are strongly encouraged to obtain, when Lightcurves for 25 main-belt asteroids were obtained at possible, the original references listed in the LCDB for their work. the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2016 July to September. 637 Chrysothemis. This Themis group member was in the field- of-view of a planned target for only one night. Without a second night, it was not possible to tell if the variations seen in the plot CCD photometric observations of 25 main-belt asteroids were were systematic rather than due to rotation of the asteroid. The made at the Center for Solar System Studies-Palmer Divide period shown in the plot is for informational purposes only. Station (CS3-PDS) from 2016 July to September. Table I lists the telescope/CCD camera combinations used for the observations. All the cameras use CCD chips from the KAF blue-enhanced family and so have essentially the same response. The pixel scales for the combinations range from 1.24-1.60 arcsec/pixel.

Desig Telescope Camera Squirt 0.30-m f/6.3 Schmidt-Cass ML-1001E Borealis 0.35-m f/9.1 Schmidt-Cass FLI-1001E Eclipticalis 0.35-m f/9.1 Schmidt-Cass STL-1001E Australius 0.35-m f/9.1 Schmidt-Cass STL-1001E Zephyr 0.50-m f/8.1 R-C FLI-1001E Table I. List of CS3-PDS telescope/CCD camera combinations.

All lightcurve observations were unfiltered since a clear filter can result in a 0.1-0.3 magnitude loss. The exposure duration varied depending on the asteroid’s brightness and sky motion. Guiding on a field star sometimes resulted in a trailed image for the asteroid. 699 Hela. Previous results for this Mars-crossing asteroid have Measurements were made using MPO Canopus. The Comp Star varied from 2.63 h (Monson, 2011) to 4.765 h (Behrend, 2003w). Selector utility in MPO Canopus found up to five comparison Most, however, have been approximately 3.3 hours (e.g., Pilcher stars of near solar-color for differential photometry. Catalog et al., 2000). The results from the PDS data in 2016 are in magnitudes were usually taken from the CMC-15 relatively good agreement with the majority of previous results. (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et al., 2009) catalogs. The MPOSC3 catalog was used as a last resort. This catalog is based on the 2MASS catalog (http://www.ipac.caltech.edu/2mass) with magnitudes converted from J-K to BVRI (Warner, 2007). The nightly zero points for the catalogs are generally consistent to about ± 0.05 mag or better, but on occasion reach 0.1 mag and more. There is a systematic offset among the catalogs so, whenever possible, the same catalog is used throughout the observations for a given asteroid. Period analysis is also done with MPO Canopus, which implements the FALC algorithm developed by Harris (Harris et al., 1989).

In the plots below, the “Reduced Magnitude” is Johnson V as indicated in the Y-axis title. These are values that have been converted from sky magnitudes to unity distance by applying –5*log (rΔ) to the measured sky magnitudes with r and Δ being, respectively, the Sun-asteroid and Earth-asteroid distances in AU. The magnitudes were normalized to the given phase angle, e.g., alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is 2083 Smither. This Hungaria asteroid had been observed by the the rotational phase ranging from –0.05 to 1.05. author on several previous occasions (Warner, 2007a; 2010; 2012a; 2015b). Each time the period was about 2.67 hours, which If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the is the same result found from the 2016 data. amplitude of the Fourier model curve and not necessarily the

Minor Planet Bulletin 44 (2017) 13

2108 Otto Schmidt. The only previous result in the LCDB for this 2919 Dali. This member of the Themis group has an estimated inner main-belt asteroid is 15.24 h (Behrend, 2001w). The period diameter of 19 km when assuming an albedo of pV ~ 0.08. Both spectrum based on the PDS data in 2016 does not support that using sparse data from the Palomar Transient Survey, Waszczak result, but favors one of 6.90 h. A period of 6.31 hour cannot be (2015) and Chang (2015) found a period of about 7.4 hours. The formally excluded. dense lightcurve from PDS in 2016 supports those results.

3443 Leetsungdao. Ivanova et al. (2002) found a period of 3.313 h for this Mars-crosser. Subsequent studies by Stephens (2002), Behrend (2001w), and Ferrero (2013) found a longer period of about 3.44 hours, as did the analysis using the 2016 PDS data.

2150 Nyctimene. This is another Hungaria asteroid that was observed by the author on several previous occasions: e.g., Warner (2007a, 6.125 h; 2008, 6.129 h; 2015a, 6.130 h). Over the course of all the apparitions, the amplitude has varied between 0.59 and 0.76 mag, indicating a spin axis pole that is mostly upright, but still has a significant obliquity. Lightcurve inversion using all the data obtained by the author from 2007 through 2016 found a pole of λ = 285°, β = –74° and sidereal period of PSID = 6.125711 h. The negative latitude indicates that the asteroid is in retrograde 4031 Mueller. This was the fourth apparition at which the author rotation. These results and those for almost 200 other Hungarias observed this Hungaria asteroid. All previous results and those will be presented in a future paper. from 2016 have a period near 2.94 h and amplitude that remained at A < 0.20 mag. Minor Planet Bulletin 44 (2017) 14

4164 Shilov. Shilov is a member of the Eunomia orbital group. It (6382) 1988 EL. Previous results by the author for this Hungaria was a target of opportunity for two nights, i.e., it was in the same include Warner (2005, 2.895 h; 2012b, 2.894 h; 2015c, 2.893 h). field as a targeted asteroid. Angeli and Barucci (1996) found a The 2016 results are in good agreement with those and other period of 18.35 h, but it is rated U = 1 (“probably wrong”) in the previous results. LCDB. The period of 18.4 hours reported here is based on a half- period solution of about 9.2 hours. This solution is rated only slightly higher, U = 2–. Future observations are encouraged.

6870 Pauldavies. Warner (2007b) and Stephens (2015) both found a period of 4.487 h. The period found from the 2016 data is essentially the same.

5427 Jensmartin. The results from the 2016 PDS data give a period of 5.813 h. This is the fourth apparition at which the author 6911 Nancygreen. This is another Hungaria observed by the observed this Hungaria and the fifth time it was worked by any author as part of a final push before doing lightcurve inversion on CS3 observer. All previous results are in close agreement with the more than 200 Hungaria asteroids. Previous results include latest period (e.g., Warner, 2009c, 5.810 h; Stephens et al., 2014a, Warner (2006, 5.3 h; 2009b, 4.33 h; 2014, 59.1 h). The mostly 5.812 h) complete lightcurve with high amplitude in 2016 virtually assures a bimodal solution with a period of about 55 h (see Harris et al., Minor Planet Bulletin 44 (2017) 15

2014). The damping time from a tumbling state to principal axis rotation for the given period and estimated diameter is about 2-4 Gyr (see Pravec et al., 2005, 2010). If there were any indications of tumbling, they were hidden within the noise and incomplete coverage of the lightcurve.

7829 Jaroff. All previous results for this Hungaria are within 0.01 h of the period found from the 2016 data (e.g., Warner and Stephens, 2009b; Stephens 2015).

(8404) 1995 AN. Previous results for this Hungaria were ambiguous. Warner (2009d) found a period of 4.612 h but one of 3.204 h could not be formally excluded. Follow-up observations in 2012 (Warner, 2012c) led to a period of 3.200 hours, as did the results from the 2016 data analysis. A period of 3.202 h is adopted for this paper.

7959 Alysecherri. In 2013, Warner (2014) reported a period of 3.161 h for this Hungaria member. The 2016 data did not support this result, with the period spectrum showing only a minor drop below the noise in the RMS values for a period near 3.16 h. The data from 2013 were forced to fit the period found using the 2016 data. While the fit is not quite as good as to 3.161 h, it is still plausible given the noise and low amplitude. A period of 3.540 hours is adopted for this paper.

Minor Planet Bulletin 44 (2017) 16

11152 Oomine. The period of 2.622 h reported here appears to be the first one for this Mars-crosser that was observed as a “full moon project.”

(28992) 2001 MW28. This inner main-belt asteroid was a target of opportunity that stayed in the same field as the planned target for several nights. There were no previous entries in the LCDB for the asteroid. (16681) 1994 EV7. The 2016 apparition was the third one at which the author observed this Hungaria. The previous results (Warner, 2007b; 2012b) are in good agreement with the period found from the 2016 data.

(43003) 1999 UC14. 1994 UC14 was another target of opportunity. The inner main-belt asteroid’s lightcurve had a small amplitude, which made finding a definitive period more difficult. The period spectrum shows several possible solutions with the one (23974) 1999 CK12. The only previously reported lightcurve at about 5.5 hours favored even though it did not have the lowest period is 5.485 h (Warner, 2012c). Masiero et al. (2012) observed RMS fit, which was near 10 hours. The shape of the lightcurve for this Hungaria with the WISE spacecraft and reported an albedo of the longer period was multimodal and asymmetric, implying a pV = 0.697 using H = 14.5. This is unusually high, but not physically improbable shape. completely unreasonable if taking into account that the WISE survey may have at times been using faulty values for H (absolute It won’t be until 2023 October that 1999 UC14 will be brighter magnitude) for many of the Hungaria members, mostly because than V ~ 17.5. Between then, most apparitions are well into the the H values were probably determined at larger phase angles and 18th and 19th magnitude range. may not have accounted for rotational variation.

If using H = 14.7 (the current value in MPCORB) and the correction algorithm from Harris and Harris (1997), pV becomes 0.61 ± 0.13. This is within 1-sigma of the average value for E-type asteroids (that of Hungaria collisional family member) as found by Warner et al. (2009). If using H = 14.8 ± 0.3 and G = 0.162 (Veres et al., 2015), pV = 0.57 ± 0.19, which is even closer to the average albedo for E-type asteroids in the LCDB.

Minor Planet Bulletin 44 (2017) 17

(96842) 1999 RH208. A middle main-belt asteroid, 1999 RH208 (45898) 2000 XQ49. The 2016 apparition was the fourth one that was in the same field as a planned target for two nights. the author observed this Hungaria asteroid. All previous results had a period near 5.42 hours (e.g., Warner 2014), making the results from 2016 in good agreement with those earlier findings.

(56591) 2000 JP37. This inner main-belt asteroid was in the field of a planned target for only one night. No period could be determined from the limited data set, though it seems probable that the period exceeds 10 hours and the amplitude was at least 0.2 mag.

(72007) 2000 XM7. There were no previously reported periods in the LCDB for this member of the Flora group, which was another target of opportunity. Fortunately, it was in the planned field for several nights, which allowed finding a reliable period estimate. Minor Planet Bulletin 44 (2017) 18

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. Group 637 Chrysothemis 07/28-07/28 53 9.9,9.9 338 0 3.7 0.3 0.06 0.01 THM 699 Hela 07/24-07/27 375 40.7,40.4 2 20 3.396 0.0005 0.16 0.01 MC 2083 Smither 07/14-07/16 213 14.9,14.4 305 19 2.675 0.001 0.11 0.01 H 2108 Otto Schmidt 07/29-08/01 135 15.0,13.8 337 0 6.9 0.05 0.16 0.01 MB-I 2150 Nyctimene 08/07-08/13 126 29.3,29.7 259 29 6.133 0.005 0.58 0.03 H 2919 Dali 08/01-08/03 179 11.6,10.9 337 0 7.43 0.01 0.45 0.02 THM 3443 Leetsungdao 07/19-07/21 93 34.1,33.7 356 7 3.439 0.005 0.47 0.03 MC 4031 Mueller 08/16-08/24 132 34.3,34.1 34 8 2.942 0.001 0.17 0.02 H 4164 Shilov 08/10-08/11 58 24.5,24.4 27 6 18.5 0.5 0.29 0.02 V 5427 Jensmartin 07/14-07/16 175 33.5,33.4 355 22 5.813 0.005 0.45 0.02 H 6382 1988 EL 08/18-08/21 109 31.8,31.7 33 10 2.904 0.002 0.2 0.03 H 6870 Pauldavies 07/11-07/13 112 28.2,27.7 335 4 4.488 0.005 0.51 0.02 H 6911 Nancygreen 08/11-08/20 421 32.9,31.2 13 16 54.7 0.5 0.75 0.05 H 7829 Jaroff 07/20-07/24 222 15.9,14.8 317 18 4.4 0.002 0.55 0.05 H 7959 Alysecherri 09/16-09/24 178 29.4,26.9 41 13 3.54 0.002 0.12 0.02 H 8404 1995 AN 09/23-09/30 149 27.9,26.6 48 19 3.202 0.001 0.14 0.01 H 11152 Oomine 07/25-08/01 210 20.7,17.7 333 0 2.622 0.001 0.1 0.01 MC 16681 1994 EV7 08/10-08/15 204 32.9,32.3 17 10 5.315 0.005 1.12 0.03 H 23974 1999 CK12 08/21-08/27 141 31.4,30.3 14 20 5.481 0.005 0.67 0.05 H 28992 2001 MW28 07/29-08/02 156 18.4,16.5 336 0 16.6 0.2 0.79 0.05 MB-I 43003 1999 UC14 07/28-08/01 119 21.3,19.3 332 0 5.459 0.006 0.12 0.01 MB-I 45898 2000 XQ49 09/16-09/18 153 25.1,24.6 35 17 5.415 0.005 1 0.03 H 56591 2000 JP37 08/14-08/14 20 30.0,30.0 25 5 0.25 MB-I 72007 2000 XM7 07/30-08/02 75 17.6,16.3 336 0 4.89 0.05 0.25 0.03 FLOR 96842 1999 RH208 08/12-08/13 56 26.6,26.5 23 11 3.236 0.006 0.36 0.03 MB-M

Table II. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude (see Harris et al., 1984), unless two values are given (first/last date in range). The Group column gives the orbital group to which the asteroid belongs. The definitions and values are those used in the LCDB (Warner et al., 2009). THM = Themis; H = Hungaria; MC = Mars-crosser; V = Vestoid; MB-I = Inner main-belt; MB-M = middle main-belt; FLOR = Flora.

The period spectrum favored a period of 3.236 h, but a solution of Rotation Periods from Palomar Transient Factory Observations.” 2.855 h cannot be formally excluded. The difference between the Ap. J. 788, A17. two is almost exactly one rotation over 24 hours. This uncertainty of the number of rotations over the span of the observations is Ferrero, A. (2013). “Rotational Period of Five Asteroids.” Minor sometimes called a rotational alias. Planet Bul. 40, 31-32.

Acknowledgements Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and Funding for PDS observations, analysis, and publication was 444 Gyptis.” Icarus 57, 251-258. provided by NASA grant NNX13AP56G. Work on the asteroid lightcurve database (LCDB) was also funded in part by National Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Science Foundation grant AST-1507535. This research was made Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, possible in part based on data from CMC15 Data Access Service H., Zeigler, K.W. (1989). “Photoelectric Observations of at CAB (INTA-CSIC) (http://svo2.cab.inta-csic.es/vocats/cmc15/) Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. and the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. This publication Harris, A.W., Harris, A.W. (1997). “On the Revision of makes use of data products from the Two Micron All Sky Survey, Radiometric Albedos and Diameters of Asteroids.” Icarus 126, which is a joint project of the University of Massachusetts and the 450-454. Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Administration and the National Science Foundation. Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., (http://www.ipac.caltech.edu/2mass/) Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics References on an asteroid lightcurve.” Icarus 235, 55-59.

Angeli, C.A., Barucci, M.A. (1996). “Rotational properties of Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, asteroids: CCD observations of nine small asteroids.” Planet. T.C., Welch, D.L. (2009). http://www.aavso.org/apass Space Sci. 44, 181-186. Ivanova, V.G., Apostolovska, G., Borisov, G.B., Bilkina, B.I. Behrend, R. (2001w, 2003w). Observatoire de Geneve web site. (2002). “Results from photometric studies of asteroids at Rozhen http://obswww.unige.ch/~behrend/page_cou.html National Observatory, Bulgaria.” Proc. ACM 2002, ESA SP 500, 505-508. Chang, C.-K., Ip, W.-H., Lin, H.-W., Cheng, Y.-C., Ngeow, C.-C., Yang, T.-C., Waszczak, A., Kulkarni, S.R., Levitan, D., Sesar, B., Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., Laher, R., Surace, J., Prince, T.A. (2014). “313 New Asteroid Nugent, C., Cabrera. (2012). “Preliminary Analysis of

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WISE/NEOWISE 3-Band Cryogenic and Post-Cryogenic Warner, B.D., Stephens, R.D. (2009b). “Lightcurve Analysis of Observations of Main Belt Asteroids.” Ap. J. Letters 759, L8. 7829 Jaroff.” Minor Planet Bul. 36, 20.

Monson, A. (2011). http://krypton.mankato.msus.edu/~monsoa1 Warner, B.D. (2009c). “Asteroid Lightcurve Analysis at the /welcome_files/Asteroid.htm Palmer Divide Observatory: 2008 May – September.” Minor Planet Bul. 36, 7-13. Pilcher, F., Warner, B.D., Goretti, V. (2000). “The Rotation Period of 699 Hela Corrected.” Minor Planet Bul. 27, 56-57. Warner, B.D. (2009d). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2008 September-December.” Minor Pravec, P., Harris, A.W., Scheirich, P., Kušnirák, P., Šarounová, Planet Bul. 36, 70-73. L., Hergenrother, C.W., Mottola, S., Hicks, M.D., Masi, G., Krugly, Yu.N., Shevchenko, V.G., Nolan, M.C., Howell, E.S., Warner, B.D. (2010). “Asteroid Lightcurve Analysis at the Palmer Kaasalainen, M., Galád, A., Brown, P., Degraff, D.R., Lambert, J. Divide Observatory: 2009 September-December.” Minor Planet V., Cooney, W.R., Foglia, S. (2005). “Tumbling asteroids.” Icarus Bul. 37, 57-64. 173, 108-131. Warner, B.D (2012a). “Asteroid Lightcurve Analysis at the Palmer Pravec, P., Scheirich, P., Durech, J., Pollock, J., Kusnirak, P., Divide Observatory: 2011 June – September.” Minor Planet Bul. Hornoch, K., Galad, A., Vokrouhlicky, D., Harris, A.W., Jehin, E., 39, 16-21. Manfroid, J., Opitom, C., Gillon, M., Colas, F., Oey, J., Vrastil, J., Reichart, D., Ivarsen, K., Haislip, J., LaCluyze, A. (2014). “The Warner, B.D (2012b). “Asteroid Lightcurve Analysis at the tumbling state of (99942) Apophis.” Icarus 233, 48-60. Palmer Divide Observatory: 2011 September – December.” Minor Planet Bul. 39, 69-80. Stephens, R.D. (2002). “Photometry of 866 Fatme, 894 Erda, 1108 Demeter, and 3443 Letsungdao.” Minor Planet Bul. 29, 2-3. Warner, B.D. (2012c). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2011 December - 2012 March.” Stephens, R.D., Coley, D., Warner, B.D. (2014). “Collaborative Minor Planet Bul. 39, 158-167. Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2013 April-June.” Minor Planet Bul. 41, 8-13. Warner, B.D. (2014). “Asteroid Lightcurve Analysis at CS3- Palmer Divide Station: 2013 June- September.” Minor Planet Bul. Stephens, R.D. (2015). “Asteroids Observed from CS3: 2015 41, 27-32. January – March.” Minor Planet Bul. 42, 200-203. Warner, B.D. (2015a). “Asteroid Lightcurve Analysis at CS3- Veres, P., Jedicke, R., Firzsimmons, A., Denneau, L., Granvik, Palmer Divide Station: 2014 June-October.” Minor Planet Bul. 42, M., Bolin, B., Chastel, S., Wainscoat, R.J., Burgett, W.S., 54-60. Chambers, K.C., Flewelling, H., Kaiser, N., Magnier, E.A., Morgan, J.S., Price, P.A., Tonry, J.L., Waters, C. (2015). Warner, B.D. (2015b). “Two New Binaries and Continuing “Absolute magnitudes and slope parameters for 250,000 asteroids Observations of Hungaria Group Asteroids.” Minor Planet Bul. observed by Pan-STARRS PS1 - Preliminary results.” Icarus 261, 42, 132-136. 34-47. Warner, B.D. (2015c). “Asteroid Lightcurve Analysis at CS3- Warner, B.D. (2005). “Asteroid lightcurve analysis at the Palmer Palmer Divide Station: 2014 December - 2015 March.” Minor Divide Observatory - winter 2004-2005.” Minor Planet Bul. 32, Planet Bul. 42, 167-172. 54-58. Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., Warner, B.D. (2006). “Asteroid lightcurve analysis at the Palmer Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., Divide Observatory: July-September 2005.” Minor Planet Bul. 33, Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light 35-39. Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry.” Astron. J. Warner, B.D. (2007a). Asteroid Lightcurve Analysis at the Palmer 150, A75. Divide Observatory - June-September 2006.” Minor Planet Bul. 34, 8-10.

Warner, B.D. (2007b). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory - December 2006 - March 2007.” Minor Planet Bul. 34, 72-77.

Warner, B.D. (2007c). “Initial Results of a Dedicated H-G Program.” Minor Planet Bul. 34, 113-119.

Warner, B.D. (2008). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: February-May 2008.” Minor Planet Bul. 35, 163-167.

Warner, B.D., Harris, A.W., Pravec, P. (2009a). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2016 July. http://www.minorplanet.info/lightcurvedatabase.html

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LIGHTCURVE ANALYSIS FOR the c-axis. This was achieved using the relation ∆m = 2.5log(a/b), TEN NEAR-EARTH ASTEROIDS as given by Burns and Tedesco (1970), where ∆m is the maximum lightcurve amplitude reached in the equatorial view. Filipe Monteiro, José Sergio Silva, Daniela Lazzaro, Plícida Arcoverde, Hissa Medeiros, Roberto Souza, Teresinha Rodrigues. It is worth mentioning that a search of the Asteroid Lightcurve Observatório Nacional, COAA, Rua Gal. José Cristino 77, Database (Warner et al., 2009, or other resources) did not find any 20921-400 Rio de Janeiro, Brazil previously reported results for these near-Earth asteroids. [email protected] (52381) 1993 HA. This NEA was observed for about ten hours on (Received: 2016 September 21) two nights from 2015 December. The composite lightcurve fits a synodic period of P = 4.107 ± 0.002 h with an amplitude of Lightcurves for ten near-Earth asteroids (NEAs) were A = 0.58 ± 0.01 mag. From this amplitude, we estimate a lower obtained at the Observatório Astronômico do Sertão de limit of a/b = 1.71, implying an elongated body. The average error Itaparica (MPC Y28, OASI) from 2015 March to 2016 on each photometric point in this and the other plots is on the May. order of 0.015 mag.

CCD photometric observations of ten NEAs were made at the Observatório Astronômico do Sertão de Itaparica (code Y28, OASI, Nova Itacuruba) between 2015 March and 2016 May. All images were obtained with the 1.0-m f/8 telescope (Astro Optik, Germany) of the IMPACTON project and an Apogee Alta U42 CCD camera (2048x2048 pixels) that was binned 2x2. This configuration gave a field-of-view of 12x12 arcmin and an image scale of 0.343 arcsec/pix. An R filter was usually used and the exposure time varied depending on the asteroid's brightness and sky motion.

Data reduction was performed using MaxIm DL following the standard procedures of flat-field correction and sky subtraction. Relative magnitudes, the difference between the instrumental (68278) 2001 FC7. Observations of this Amor asteroid were magnitude of the asteroid and a field comparison star with similar obtained for about five hours during one night, 2015 September magnitude, were computed to obtain the lightcurves. The rotation 10. The phased lightcurve curve fits a period of P = 4.230 ± period was then derived using Fourier analysis (e.g. Harris et al., 0.002 h, although some rotation phases are not covered by the 1989). On some nights, due to the rapid movement of the asteroid, observations. Moreover, it is very asymmetric, showing some the field of observations, and consequently the comparison star, dispersion among the points. The amplitude is 0.22 ± 0.02 mag. changed during the night. In these cases, the analysis considered the observations with different comparison star as distinct individual lightcurves. In the figures below, this is represented by points of different color on a same date.

The observational circumstances for each of the observed asteroids are given in Table I along with the results, which are discussed individually below. In this table we give for each obtained rotation period a reliability code (Warner et al., 2009). A period with code 1 is based on inconclusive coverage and may be completely wrong; 2 corresponds to a reasonably secure result, probably not wrong by more than 10-20%; 3 indicates a secure result. Besides deriving the rotation period, the maximum lightcurve amplitude was used to estimate the a/b ratio for a triaxial ellipsoid asteroid shape with a > b > c and rotation about

Number Name yyyy mm/dd Exp Phase LPAB BPAB Period P.E. Amp A.E. U 52381 1993 HA 2015 12/08-12/09 120 47.2,47.4 81 -30 4.107 0.002 0.58 0.01 3 68278 2001 FC7 2015 09/10-09/10 80 30.9 323 -6 4.230 0.002 0.22 0.02 2 138847 2000 VE62 2016 03/11-05/09 60 53.6,56.0 238 10 6.469 0.002 0.36 0.02 3 163243 2002 FB3 2016 03/10-04/03 50 53.3,54.8 137 -28 6.231 0.001 0.19 0.02 2 315098 2007 EX 2016 05/02-05/05 100 54.0,54.8 184 -37 2.447 0.003 0.20 0.02 3 337069 1998 FX134 2015 05/14-05/17 80 16.4,16.6 236 -13 7.487 0.001 0.46 0.02 3 425713 2011 BK24 2015 04/18-04/18 80 15.5 206 -11 6.010 0.002 0.24 0.02 3 1998 GL10 2015 03/14-03/26 80 12.0,5.3 180 -5 5.930 0.001 0.10 0.02 2 2015 CA1 2015 03/13-03/20 80 31.1,38.2 200 -5 2.949 0.002 0.49 0.02 3 2016 HL 2016 05/06-05/08 100 9.8,11.2 220 -2 2.930 0.002 0.15 0.02 2

Table I. Observing circumstances. Exp is average exposure time, seconds. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude. The U rating is our estimate and not necessarily the one assigned in the asteroid lightcurve database (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 21

(138847) 2000 VE62. We observed this asteroid, a member of the (337069) 1998 FX134. We observed this Amor asteroid for more Amor class, for almost 12 hours on five nights during 2016 than 17 hours on four nights during 2015 May. The 6th-order March, April, and May. The composite lightcurve fits a period of Fourier fit to the data revealed a period of P = 7.487 ± 0.001 h. P = 6.469 ± 0.002 h using a 5th-order Fourier fit with an amplitude The composite lightcurve is double-peaked and gives good of 0.36 ± 0.02 mag. It is important to note that it was possible to coverage from the four nights. An amplitude of 0.46 ± 0.02 mag use all the lightcurves observed to build the composite lightcurve suggests an elongated shape, with a/b ≥ 1.53. because the phase angle remained virtually unchanged during the observing interval.

(425713) 2011 BK24. We observed this Amor asteroid for about five hours on the night of 2015 April 18. The phased lightcurve (163243) 2002 FB3. This Aten class and potentially hazardous fits a period of P = 6.010 ± 0.002 h with an amplitude of 0.24 ± asteroid (PHA) was discovered at LINEAR, New Mexico, on 2002 0.02 mag. Although these values have been determined from just March 18. We observed this asteroid for a total of nearly ten hours one night of observations, we consider the period well-established. on four nights during 2016 March and April. The composite The composite lightcurve is asymmetric, with the primary lightcurve with a 5th-order Fourier fit gives a period of 6.231 ± maximum being much larger than the secondary one. 0.001 h. Although not complete, the lightcurve has two maxima and minima and a small amplitude of A = 0.19 ± 0.02 mag.

1998 GL10. Observations of this Amor asteroid were made for about 22 hours on five nights from 2015 March 14 to 26. The (315098) 2007 EX. Observations of this Aten asteroid were made composite lightcurve fits a period of P = 5.930 ± 0.001 h. It is on four nights, 2016 May 2-5, for almost ten hours. The composite quite asymmetric, showing a high dispersion and small amplitude lightcurve fits a period of P = 2.447 ± 0.003 h. It was obtained (0.10 ± 0.02 mag), but has good coverage. Additional observations with a 4th-order Fourier fit and shows some dispersion among the are needed to confirm the derived period. points. The composite lightcurve clearly shows two maxima and two minima along with a small amplitude of A = 0.20 ± 0.02 mag.

2015 CA1. We observed this Amor asteroid for almost five hours on three nights during 2015 March. The phased curve fits a period of P = 2.949 ± 0.002 h. This composite lightcurve is relatively Minor Planet Bulletin 44 (2017) 22 well-covered and presents a low dispersion of the data. It is Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid asymmetric and the amplitude of 0.49 ± 0.02 mag implies Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sept. a/b ≥ 1.57, suggesting an elongated object. http://www.minorplanet.info/lightcurvedatabase.html

NEAR-EARTH ASTEROID LIGHTCURVE ANALYSIS AT CS3-PALMER DIVIDE STATION: 2016 JULY-SEPTEMBER

Brian D. Warner Center for Solar System Studies / MoreData! 446 Sycamore Ave. Eaton, CO 80615 USA [email protected]

(Received: 2016 October 3)

2016 HL. The Apollo class and potentially hazardous asteroid Lightcurves for 46 near-Earth asteroids (NEAs) obtained (PHA) 2016 HL was discovered at SONEAR Observatory, at the Center for Solar System Studies-Palmer Divide Oliveira-Brazil, on 2016 April 19. An extremely close approach to Station (CS3-PDS) from 2016 July-September were the Earth (0.05 AU) occurred on April 12. We observed this analyzed for rotation period and signs of satellites or asteroid after its close approach for about 8.5 hours on three tumbling. nights, 2016 May 6 to 8. The derived synodic period is P = 2.930 ± 0.002 h with a small amplitude of A = 0.15 ± 0.02 mag. CCD photometric observations of 46 near-Earth asteroids (NEAs) were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2016 July-September. Table I lists the telescope/CCD camera combinations used for the observations. All the cameras use CCD chips from the KAF blue-enhanced family and so have essentially the same response. The pixel scales for the combinations range from 1.24-1.60 arcsec/pixel.

Table I. List of CS3-PDS telescope/CCD camera combinations. Acknowledgements All lightcurve observations were unfiltered since a clear filter can The authors acknowledge CAPES for the fellowships and result in a 0.1-0.3 magnitude loss. The exposure duration varied FAPERJ for the support to D.L., through project number E-26- depending on the asteroid’s brightness and sky motion. Guiding 102.967/2011. Finally, we are gratefully to the IMPACTON team, on a field star sometimes resulted in a trailed image for the in particular, A. Santiago, for the technical support at OASI. asteroid. If necessary, an elliptical aperture with the long axis parallel to the asteroid’s path was used. References Measurements were made using MPO Canopus. The Comp Star Burns, J.A., Tedesco, E.F. (1979). “Asteroid Lightcurves – Results Selector utility in MPO Canopus found up to five comparison for Rotations and Shapes.” in Asteroids (T. Gehrels, editor), pp stars of near solar-color for differential photometry. Catalog 494-527. Univ. Arizona Press, Tucson. magnitudes were usually taken from the CMC-15 (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et Harris, A.W., Young, J.W. (1983). “Asteroids rotation. IV.” al., 2009) catalogs. The MPOSC3 catalog was used as a last Icarus 54, 59-109. resort. This catalog is based on the 2MASS catalog (http://www.ipac.caltech.edu/2mass) with magnitudes converted Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., from J-K to BVRI (Warner, 2007). The nightly zero points for the Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, catalogs are generally consistent to about ± 0.05 mag or better, but H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, on occasion reach 0.1 mag and more. There is a systematic offset 24, 60, 261, and 863.” Icarus 77, 171-186. among the catalogs so, whenever possible, the same catalog is used throughout the observations for a given asteroid. Period Pravec, P., Harris, A.W., Michalowski, T. (2002). “Asteroid analysis is also done with MPO Canopus, which implements the Rotations.” in Asteroids III (W.F. Bottke, A. Cellino, P. Paolicchi, FALC algorithm developed by Harris (Harris et al., 1989). R.P. Binzel, eds.) pp 113-122. Univ. Arizona Press, Tucson. In the plots below, the “Reduced Magnitude” is Johnson V as indicated in the Y-axis title. These are values that have been

Minor Planet Bulletin 44 (2017) 23 converted from sky magnitudes to unity distance by applying 1863 Antinous. Binzel (1987) first reported a period of 4.02 h. –5*log (rΔ) to the measured sky magnitudes with r and Δ being, Harris et al. (1999) observed the asteroid at about the same time in respectively, the Sun-asteroid and Earth-asteroid distances in AU. 1982 and found a period of 4.386 h. Observations by Pravec et al. The magnitudes were normalized to the given phase angle, e.g., (1999w) led to a more reliable solution of 7.4568 h. The NEA was alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is observed at CS3-PDS in early 2016 (Warner, 2016a; 7.453 h). The the rotational phase, ranging from –0.05 to +1.05. latest PDS observations made in 2016 August led to a period of 7.471 h, which is consistent with the Pravec et al. and earlier PDS For the sake of brevity, only some of the previously reported results. results may be referenced in the discussions on a specific asteroid. For a more complete listing, the reader is directed to the asteroid lightcurve database (LCDB; Warner et al., 2009). The on-line version at http://www.minorplanet.info/lightcurvedatabase.html allows direct queries that can be filtered a number of ways and the results saved to a text file. A set of text files of the main LCDB tables, including the references with bibcodes, is also available for download. When possible, readers are strongly encouraged to check against the original references listed in the LCDB.

If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the amplitude of the Fourier model curve and not necessarily the adopted amplitude for the lightcurve. The value is provided as a matter of convenience.

433 Eros. This well-known and extensively studied NEA was observed twice at PDS in 2016, first in July and then in late August. During the approximately six-week interval between data 2100 Ra-Shalom. The period for Ra-Shalom was first established sets, the lightcurve shape and amplitude evolved significantly as at 19.79 h by Ostro et al. (1984). The period found from the 2016 the asteroid went from phase angle 28° to 10°. The lower PDS data is slightly longer, 19.89 h, but still consistent with amplitude at a lower phase angle is a well-established trait of most earlier results. asteroid lightcurves (Zappala et al., 1990).

3352 McAuliffe. This is a suspected binary asteroid (Warner, 2012). No signs of the purported satellite were seen at the 2016 apparition.

Minor Planet Bulletin 44 (2017) 24

5143 Heracles. This is a known binary (Taylor et al., 2012b) based on radar observations. The estimated effective diameter ratio is about 0.16 and the orbital period in the range of 14-17 hours. The small size ratio is on the edge of being detectable with photometry observations alone, so it is not too surprising that the satellite had not been discovered before the radar observations.

(7341) 1991 VK. Pravec et al. (1998) found a period of 4.2096 h. The period of 4.211 h derived from the 2016 PDS data is consistent with that earlier result.

It’s of some note that the AKARI survey (Usui et al., 2011) reported a very high albedo, pV = 0.625, which is somewhat unusual within the NEA population. Even if using a different (5587) 1990 SB. Koff et al. (2002) did an extensive study of absolute magnitude, H =16.95 (Pravec et al., 2012), and the 1990 SB that included observations from before and after correcting algorithm of Harris and Harris (1997), the albedo is still opposition. This allowed showing the evolution of the lightcurve 0.49 ± 0.10. This is more consistent with type E (possibly type M) shape and synodic period over several months. The period found asteroids (Warner et al., 2009a) rather than the more typical S- from the 2016 PDS data is consistent with the average period from complex or, to a lesser extent, C-complex types seen among the Koff et al. and other previous results. NEA population.

The asteroid has a very favorable apparition in 2017 February, at which time it will be a strong radar target. Supporting photometric observations are encouraged. The close encounter may also allow spectroscopic observations of the asteroid that will help determine its true taxonomic class.

(5836) 1993 MF. The period of 4.953 h found from the PDS data is consistent with earlier results such as Mottola et al. (1995; 4.959 h) and Pravec et al. (1997w; 4.9543 h). The NEA was observed in 2016 June (Warner, 2016c; 4.948 h) when the amplitude was 0.82 mag. The 0.88 mag found in September is the largest found in the LCDB for 1993 MF. (7888) 1993 UC. The PDS observations in 2016 led to a period of 2.337 h, which is consistent with the 2.340 h found by Pravec et al. (1996). Unfortunately, there appears to be no results between these two, making it difficult – if not impossible – to determine if the rotation period is being affected by YORP.

Minor Planet Bulletin 44 (2017) 25

shadowing effects can come into play. The period agrees with Pravec et al. (2000w; 9.345h) and Stephens (2013w; 9.374 h).

(10636) 1998 QK56. The results from PDS appear the first to be reported for this NEA. The asteroid has a favorable apparition in 2017 March, when it will reach V ~ 15.2 mag. Follow-up observations at PDS are planned. Other observations are (40263) 1999 FQ5. There were no other periods in the LCDB for encouraged. 1999 FO5. The next favorable apparition is not until 2036.

(162117) 1998 SD15. There were no previously reported periods (52750) 1998 KK17. Higgins (2005) reported a period of 3.124 h in the LCDB for 1998 SD15. The 2016 apparition was the last for this NEA while the author (Warner, 2015) reported 2.28 h. good chance for photometric observations until 2025 September, Neither of these fit the single period analysis of the data. when the asteroid will reach V ~ 17.0. Before then, it is mostly below 20th magnitude.

A plot of the raw data from late August to early September showed indications of a long period with, possibly, a short-period component as well. On this presumption, a dual-period search was (16834) 1997 WU22. The usual lightcurve shape for 1997 WU22 done using MPO Canopus where a solution for a long period was may have been due in good part to the high phase angle, when found and then subtracted from the data to determine if there was

Minor Planet Bulletin 44 (2017) 26 a short period. The short period was subtracted to confirm the long Note that the short period is very close to the one found by period. The process continued until both periods stabilized. The Higgins. It’s possible that by using arbitrary zero-point results are shown in the four plots, two being period spectra and adjustments, the long period was unintentionally removed, which the others the individual components of the combined lightcurve. serves as a cautionary tale to “let the data fall where they may” until there is good reason to do otherwise.

1998 KK17 may be another example of a so-called very wide binary asteroid. See Warner (2016b) for a discussion of this suspected subclass of binary asteroids.

(68346) 2001 KZ66. Based on radar observations, Benner et al. (2006) estimated a rotation period of about 2.7 hours. Subsequent photometric observations by the author in 2016 May (Warner, 2016c) found a more likely period of 4.987 h. The more recent PDS data, obtained in 2016 July, support the longer period, though it may need further refinement at the next favorable apparition (2022, V ~ 18.4).

(87684) 2000 SY2. Higgins (2005) found a period of 8.80 hours. The 2016 PDS data do not support that result, but favor one of 2.8712 h.

Minor Planet Bulletin 44 (2017) 27

(106538) 2000 WK63. This appears to be the first reported period (162117) 1998 SD15, (163348) 2002 NN4. These are the first for 2000 WK63. The next good chance to obtain follow-up data reported results in the LCDB for these two NEAs. comes in 2020 March.

Based on times to dampen from tumbling (non-principal axis rotation) to single axis rotation (Pravec et al., 2014, and references therein), there is a reasonable chance that this asteroid should be tumbling. There were no obvious signs of tumbling, e.g., the slope of the data on a given night not following the slope of the Fourier curve. A better judgement of tumbling would require following the asteroid through at least another quarter rotation to see if the lightcurve repeated itself within the data noise level.

(154244) 2002 KL6. Koehn et al. (2014) followed this NEA for several months in 2009. The approximate average of the several synodic periods was 4.608 h, which is essentially identical to the period found with the 2016 PDS data.

(250458) 2004 BO41. There were no previously reported periods for 2004 BO41 in the LCDB. There were several solutions, each commensurate with an Earth day. However, the best solution, based on the slopes of the lightcurve, is for a period of 16.19 h.

Minor Planet Bulletin 44 (2017) 28

(257838) 2000 JQ66. Using observations from 2000, Pravec et al. (370307) 2002 RH52. The period found from the 2016 PDS data (2000w) found a period of 11.1 hours. The PDS data from 2016 agrees well with the one of 4.222 h found by Pravec et al. led to a consistent and slightly more refined result of 11.094 h. (2003w).

(347813) 2002 NP1, (357024) 1999 YR14. There were no (385343) 2002 LV. Pravec et al. (2002w) and Hicks et al. (2009w) previous entries in the LCDB for 2002 NP1 and 1999 YR14. both reported a period of about 6.20 h. The results from the PDS observation agree with that period.

Spectroscopic observations by Thomas et al. (2014) determined that 2002 NP1 is a type Q asteroid on the Bus-DeMeo taxonomic (452389) 2002 NW16. There were no previous results in the system (DeMeo et al., 2009, and references therein). The Q LCDB to help guide finding the period for 2002 NW16. The asteroids, 1862 Apollo being one of the well-known members, are period appears commensurate with an Earth day. Based on a half- uncommon among the inner main-belt. They are an “outlier” class period solution and the reasonable slopes of the Fourier curve, a in the Bus-DeMeo system, being an intermediate type between the period of 46.7 h is adopted for this paper. The amplitude of 0.67 Vestoids (V) and much more common S-complex. mag could be off significantly from the true value.

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(464797) 2004 FZ1. This appears to be another example of a very (467336) 2002 LT38. This appears to be the first published period wide binary asteroid. The lightcurve for these objects consists of a for 2002 LT38. Even when assuming a longer damping time from long-period component with an amplitude A > 0.3 mag and a tumbling to single axis rotation (Pravec et al., 2014, and short-period component with a smaller amplitude, usually references therein), the 21.8 hour period found here makes this a A < 0.15 mag. The primary body is presumed to the one with the likely tumbler candidate. There may be some indications of long period. See Warner (2016b) for more about these asteroids. tumbling in the lightcurve, for example, the “break” in the Fourier curve around 0.45 rotation phase.

(468448) 2003 LS3. This NEA was observed twice at PDS in 2016. The first time was in July, when a period of 5.325 h and amplitude of 0.32 mag were found. The phase angle was about 23°. About six weeks later, the synodic period was statistically the same, but the amplitude had dropped to 0.23 mag, which was expected due to the lower phase angle of about 8°.

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(469513) 2003 QR79, (469634) 2004 SZ19, (470510) 2008 (471241) 2011 BX18. CJ116. These look to be the first reported periods for the three NEAs. The low amplitude and significant noise in the lightcurve for 2003 QR79 make the solution less than secure, but it is still a reasonable estimate. The gap in the lightcurve for 2004 SZ19 is partly due to the adopted period being commensurate with an Earth day. Every 48 hours, approximately the same part of the lightcurve was covered. The gap was outside the observing window between the asteroid rising and setting or start of twilight.

The period for 2008 CJ116 makes it a good candidate for being a tumbler. However, there were no obvious signs in the data set. See Pravec et al. (2005) for a detailed discussion of tumbling asteroids.

The high phase angle at which the observations of 2011 BX18 were made introduced the likelihood of strong shadowing effects that would produce an atypical lightcurve. Combined with possible solutions commensurate with an Earth day, a definitive solution could not be found. The period spectrum favored 4.828 hours. However, as seen in the alternate lightcurve, the data fit almost as well to a period of 4.023 h. The two periods represent a difference of almost exactly one rotation over 24 hours.

Minor Planet Bulletin 44 (2017) 31

1999 SO5. While the period spectrum allows for several possible Unfortunately, the 2016 apparition was the last time the asteroid solutions, the dominant one is the most physically plausible (see will be brighter than V ~ 21 through 2050. Harris et al., 2014). The alternate solutions represent either the half-period or integral multiples of the half-period greater than the adopted period of 1.380 hours.

2005 TF. This is the first reported period for 2005 TF.

2009 ES. The very high noise in the data makes any solution suspect. However, there did appear to be two components to the lightcurve, making it another potential very wide binary candidate (see Warner, 2016b). For the long period, the period spectrum settled between 25 and 30 hours, with 28.1 h adopted here. It’s hardly conclusive. Subtracting the resulting Fourier model curve produces a relatively convincing solution of 2.988 h, despite the noise being nearly greater than the amplitude.

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2013 TV5. The maximums of the lightcurve for 2013 TV are not 2016 NA1. The period of 8.67 hours adopted here is considered a 0.5 rotation phase apart, but the minimums nearly are. Such “best guess” given the low amplitude and noisy data set. The asymmetry is not impossible, especially at higher phase angles. period spectrum offered little help, showing a number of nearly However, it does make the solution at least somewhat suspect. likely solutions.

2016 PN1. This asteroid faded from view too soon, and so it was not possible to get a more complete data set. The period of 76 hours is a best fit to the data, but it is likely wrong.

On the other hand, the period spectrum shows only a few obvious possibilities and the longer periods produce physically improbable lightcurves with multiple maximum/minimum pairs.

2014 KD91. There were no previously reported periods in the LCDB for 2014 KD91. Given the extensive coverage of the lightcurve and time span of the observations, the period is considered secure despite the low amplitude and somewhat noisy data set.

2016 RB1. The estimated diameter of only 7 meters made 2016 RB1 an excellent candidate for being a super-fast rotator (P < 1 hour). For this reason, exposures were kept to 10 seconds in order to avoid rotational smearing (see Pravec et al., 2000). This would work only if the rotation period was greater than about 50 seconds.

The raw lightcurve showed what appeared to be just noise but, given the possibility for a very short period, a search was made from 0.001 to 2.5 hours in 0.001 h steps. This lead to the

approximate period of 0.027 h, which was further refined to 0.02674 h. Minor Planet Bulletin 44 (2017) 33

2016 NG33. A period of 2.321 hours is adopted for this paper. However, as the period spectrum shows, a number of other solutions are possible. The amplitude of 0.25 mag lends support to the adopted period (see Harris et al., 2014).

2016 RP33. There were no previous entries in the LCDB for this NEA.

2016 NH15. The adopted period of 52.6 h makes this a good tumbling candidate. The data set was too limited and noisy to see any obvious signs of tumbling.

2016 LX48. Initial analysis of the data set led to a solution of about 3.8 hours, which produced a bimodal lightcurve. At large phase angles, this is not always a good assumption. Soon after the PDS observations, Amadeo Aznar in Spain also made observations of the asteroid. His analysis showed that a period of about 5.5 hours was more likely (Aznar, private communications).

Another search was made with the PDS data set, which led to the adopted period of 5.669 h for this paper, despite the unusual shape of the lightcurve and the fact that the PDS data fit almost as well to the 3.8 hour period.

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Asteroid 2005 CR37: Radar images and photometry of a candidate contact binary.” Icarus 182, 474-481.

Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.” Icarus 72, 135-208.

DeMeo, F.E., Binzel, R.P., Slivan, S.M., Bus, S.J. (2009). “An Extension of the Bus Asteroid Taxonomy into the Near-Infrared.” Icarus 202, 160-180.

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Harris, A.W., Harris, A.W. (1997). “On the Revision of Radiometric Albedos and Diameters of Asteroids.” Icarus 126, 2016 CL264. There were no previous entries in the LCDB for this 450-454. NEA. The sparse coverage of the lightcurve makes the period less than certain. However, as with some earlier cases, a search on Harris, A.W., Young, J.W., Bowell, E., Tholen, D.J. (1999). half-periods and the slopes of the Fourier curve make the adopted “Asteroid Lightcurve Observations from 1981 to 1983.” Icarus period a good “best estimate.” 142, 173-201. Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics on an asteroid lightcurve.” Icarus 235, 55-59.

Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). http://www.aavso.org/apass

Hicks, M, Rhoades, H., Somers, J., Grote, M. (2009w). Astronomer's Telegram 2134. http://www.astronomerstelegram.org

Higgins, D.J. (2005). “Lightcurve and period determination for 479 Caprera, 2351 O'Higgins (36378) 2000 OL19, (52750) 1998 KK17, (87684) 2000 SY2.” Minor Planet Bul. 32, 36-38.

Koehn, B.W., Bowell, E.L.G., Skiff, B.A., Sanborn, J.J., Acknowledgements McLelland, K.P., Pravec, P., Warner, B.D. (2014). “Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) - Thanks to Amado Aznar for his comments and suggestions 2009 January through 2009 June.” Minor Planet Bul. 41, 286-300. regarding 2016 LX48. Koff, R.A., Pravec, P., Sarounova, L., Kusnirak, P., Brincat, S., Funding for PDS observations, analysis, and publication was Goretti, V., Sposetti, S., Stephens, R., Warner, B. (2002). provided by NASA grant NNX13AP56G. Work on the asteroid Collaborative Lightcurve Photometry of Asteroid (5587) 1990 lightcurve database (LCDB) was also funded in part by National SB.” Minor Planet Bul. 29, 51-53. Science Foundation grant AST-1507535. Mottola, S., De Angelis, G., Di Martino, M., Erikson, A., Hahn, This research was made possible in part based on data from G., Meukum, G. (1995). “The near-earth objects follow-up CMC15 Data Access Service at CAB (INTA-CSIC) program: First results.” Icarus 117, 62-70 (http://svo2.cab.inta-csic.es/vocats/cmc15/) and the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Ostro, S.J., Harris, A.W., Campbell, D.B., Shapiro, I.I., Young, J. Martin Ayers Sciences Fund. (1984). “Radar and photoelectric observations of asteroid 2100 Ra-Shalom.” Icarus 60, 391-403. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Pravec, P., Sarounova, L., Wolf, M. (1996). “Lightcurves of 7 Massachusetts and the Infrared Processing and Analysis Near-Earth Asteroids.” Icarus 124, 471-482. Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Pravec, P., Wolf, M., Sarounova, L. (1998). “Lightcurves of 26 Foundation. (http://www.ipac.caltech.edu/2mass/) Near-Earth Asteroids.” Icarus 136, 124-153.

References Pravec, P., Wolf, M., Sarounova, L. (1997w, 1999w, 2000w, 2002w, 2003w). http://www.asu.cas.cz/~ppravec/neo.htm Benner, L.A.M., Nolan, M.C., Ostro, S.J., Giorgini, J.D., Pray, D.P., Harris, A.W., Magri, C., Margot, J.-L. (2006). “Near-Earth Minor Planet Bulletin 44 (2017) 35

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. Grp 433 Eros 07/04-07/06 223 28.8,28.2 326 2 5.271 0.001 0.47 0.01 NEA 433 Eros 08/29-08/31 1272 9.2,10.4 329 9 5.270 0.001 0.33 0.01 NEA 1863 Antinous 08/06-08/10 159 42.6,40.2 7 0 7.471 0.005 0.33 0.02 NEA 2100 Ra-Shalom 08/10-08/20 287 57.2,54.5 12 4 19.89 0.05 0.55 0.03 NEA 3352 McAuliffe 09/25-09/27 156 23.2,22.5 34 -7 2.212 0.002 0.12 0.02 NEA 5143 Heracles 09/12-09/17 133 31.4,31.8 52 11 2.704 0.002 0.15 0.03 NEA 5587 1990 SB 08/05-08/10 129 38.4,37.2 23 2 5.0520 0.0005 0.70 0.02 NEA 5836 1993 MF 09/09-09/11 212 45.9,44.7 31 11 4.953 0.005 0.88 0.02 NEA 7341 1991 VK 09/05-09/08 142 20.8,19.5 8 8 4.211 0.003 0.21 0.03 NEA 7888 1993 UC 09/09-09/15 109 42.4,44.4 52 -25 2.337 0.002 0.16 0.02 NEA 10636 1998 QK56 09/12-09/15 163 2.7,0.2 353 0 9.84 0.01 0.32 0.03 NEA 16834 1997 WU22 08/06-08/10 365 79.9,74.2 275 38 9.343 0.005 0.60 0.02 NEA 40263 1999 FQ5 08/29-09/11 211 48.6,46.3 25 -8 28.00 0.05 0.27 0.03 NEA 52750 1998 KK17 08/26-09/08 259 47.6,54.0 29 -14 26.43 0.05 0.24 0.01 NEA 68346 2001 KZ66 07/17-07/19 123 67.3,69.3 269 46 4.996 0.003 0.35 0.02 NEA 87684 2000 SY2 08/22-09/04 216 59.5,51.8 32 -13 2.8712 0.0004 0.09 0.01 NEA 106538 2000 WK63 08/21-09/01 224 64.8,52.4 278 11 51.2 0.2 0.60 0.04 NEA 154244 2002 KL6 09/09-09/11 210 40.9,38.7 14 7 4.609 0.005 0.92 0.02 NEA 162117 1998 SD15 09/12-09/15 402 71.2,62.5 345 40 7.33 0.01 0.26 0.03 NEA 163348 2002 NN4 08/04-08/09 196 20.2,19.9,20.6 316 14 14.50 0.03 0.74 0.05 NEA 250458 2004 BO41 09/15-09/28 1398 85.2,61.6 330 39 16.19 0.01 0.85 0.05 NEA 257838 2000 JQ66 07/03-07/08 254 38.0,12.4,36.8 281 15 11.094 0.005 0.63 0.03 NEA 347813 2002 NP1 08/02-08/05 177 29.1,27.4 337 6 5.915 0.005 0.86 0.03 NEA 357024 1999 YR14 08/30-09/01 1085 57.7,63.9 7 -16 4.2477 0.0005 1.19 0.03 NEA 370307 2002 RH52 09/23-09/27 171 36.0,36.3 37 9 4.218 0.003 0.78 0.03 NEA 385343 2002 LV 07/03-07/05 138 36.4,37.3 254 36 6.20 0.01 0.51 0.03 NEA 452389 2002 NW16 07/07-07/16 196 67.5,65.8 334 0 46.7 0.2 0.65 0.05 NEA 464797 2004 FZ1 08/11-08/17 1754 51.1,31.6 338 26 45.4 0.2 0.39 0.03 NEA 467336 2002 LT38 06/27-07/06 391 66.2,87.2 238 14 21.80 0.05 1.16 0.05 NEA 468448 2003 LS3 07/05-07/08 146 23.7,23.2 299 16 5.325 0.005 0.32 0.02 NEA 468448 2003 LS3 08/23-08/25 148 8.5,8.3 327 4 5.329 0.005 0.02 0.02 NEA 469513 2003 QR79 09/02-09/04 95 11.4,15.3 335 7 4.11 0.01 0.18 0.03 NEA 469634 2004 SZ19 08/25-08/28 234 31.3,28.0 353 13 16.39 0.03 0.34 0.04 NEA 470510 2008 CJ116 12/31-12/31 445 31.3,0.0,28.0 0 0 32.26 0.01 1.00 0.03 NEA 471241 2011 BX18 08/05-08/09 337 73.0,61.3 356 14 4.828 0.005 0.27 0.02 NEA 1999 SO5 09/28-09/30 194 29.1,26.4 24 5 1.380 0.001 0.73 0.03 NEA 2005 TF 09/28-10/02 163 15.8,13.9 18 -3 2.57 0.005 0.29 0.03 NEA 2009 ES 09/10-09/14 960 37.2,44.3 332 16 28.0 0.5 0.33 0.04 NEA 2013 TV5 09/27-09/28 287 41.6,43.4 340 12 0.8367 0.0002 0.42 0.03 NEA 2014 KD91 09/13-09/26 250 31.3,25.8 19 19 2.829 0.001 0.15 0.02 NEA 2016 NA1 08/02-08/04 268 13.5,15.6 317 7 8.67 0.05 0.14 0.04 NEA 2016 PN1 09/03-09/09 342 38.4,35.1 10 6 76 1 0.16 0.03 NEA 2016 RB1 09/07-09/07 422 0.0,0.0 0 0 0.02674 0.00001 0.18 0.03 NEA 2016 NH15 07/25-07/31 230 13.6,14.3 309 9 52.6 0.5 0.29 0.04 NEA 2016 NG33 08/05-08/06 205 36.9,35.3 335 -3 2.321 0.003 0.25 0.04 NEA 2016 RP33 09/18-09/24 411 4.6,6.6 357 1 4.682 0.002 0.15 0.03 NEA 2016 LX48 09/09-09/11 614 85.5,79.1 312 27 5.669 0.002 0.45 0.03 NEA 2016 CL264 08/07-08/10 601 102.5,75.9 93 -9 19.9 0.1 0.57 0.05 NEA

Table III. Observing circumstances. Pts is the number of data points used in the analysis. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are, respectively the average phase angle bisector longitude and latitude, unless two values are given (first/last date in range). Grp is the orbital group of the asteroid. See Warner et al. (LCDB; 2009; Icarus 202, 134-146.).

Pravec, P., Harris, A.W., Scheirich, P., Kušnirák, P., Šarounová, Reichart, D., Ivarsen, K., Haislip, J., LaCluyze, A. (2014). “The L., Hergenrother, C.W., Mottola, S., Hicks, M.D., Masi, G., tumbling state of (99942) Apophis.” Icarus 233, 48-60. Krugly, Yu.N., Shevchenko, V.G., Nolan, M.C., Howell, E.S., Kaasalainen, M., Galád, A., Brown, P., Degraff, D.R., Lambert, J. Stephens, R.D. (2013w). V., Cooney, W.R., Foglia, S. (2005). “Tumbling asteroids.” Icarus http://www.planetarysciences.org/PHP/CS3_Lightcurves.php 173, 108-131. Taylor, P., Nolan, M.C., Howell, E.S. (2012) CBET 3176. Pravec, P., Harris, A.W., Kusnirak, P., Galad, A., Hornoch, K. (2012). “Absolute magnitudes of asteroids and a revision of Thomas, C.A., Emery, J.P., Trilling, D.E., Delbo, M., Hora, J.L., asteroid albedo estimates from WISE thermal observations.” Mueller, M. (2014). Physical characterization of Warm Spitzer- Icarus 221, 365-387. observed near-Earth objects.” Icarus 228, 217-246.

Pravec, P., Scheirich, P., Durech, J., Pollock, J., Kusnirak, P., Usui, F., Kuroda, D., Müller, T.G., Hasegawa, S., Ishiguro, M., Hornoch, K., Galad, A., Vokrouhlicky, D., Harris, A.W., Jehin, E., Ootsubo, T., Ishihara, D., Kataza, H., Takita, S., Oyabu, S., Ueno, Manfroid, J., Opitom, C., Gillon, M., Colas, F., Oey, J., Vrastil, J., M., Matsuhara, H., Onaka, T. (2011). “Asteroid Catalog Using

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Akari: AKARI/IRC Mid-Infrared Asteroid Survey.” Pub. Ast. Soc. Warner, B.D. (2016a). “Near-Earth Asteroid Lightcurve Analysis of Japan 63, 1117-1138. at CS3-Palmer Divide Station: 2016 January-April.” Minor Planet Bul. 43, 240-250. Warner, B.D. (2007). “Initial Results of a Dedicated H-G Program.” Minor Planet Bull. 34, 113-119. Warner, B.D. (2016b). Three Additional Candidates for the Group of Very Wide Binary Asteroids.” Minor Planet Bul. 43, 306-309. Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Last update: 2016 Warner, B.D. (2016c). “Near-Earth Asteroid Lightcurve Analysis Feb. http://www.minorplanet.info/lightcurvedatabase.html at CS3-Palmer Divide Station: 2016 April-July.” Minor Planet Bul. 43, 311-319. Warner, B.D. (2012). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2011 December - 2012 March.” Minor Planet Zappala, V., Cellini, A., Barucci, A.M., Fulchignoni, M., Bul. 39, 158-167. Lupishko, D.E. (1990). “An analysis of the amplitude-phase relationship among asteroids.” Astron. Astrophys. 231, 548-560. Warner, B.D. (2015). Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2015 March-June.” Minor Planet Bul. 42, 256-266.

LIGHTCURVE ANALYSIS OF HILDA ASTEROIDS Telescopes Cameras AT THE CENTER FOR SOLAR SYSTEM STUDIES: 0.30-m f/6.3 Schmidt-Cass FLI Microline 1001E 2016 JUNE-SEPTEMBER 0.35-m f/9.1 Schmidt-Cass FLI Proline 1001E 0.35-m f/11 Schmidt-Cass SBIG STL-1001E Brian D. Warner 0.40-m f/10 Schmidt-Cass 0.50-m f/8.1 Ritchey-Chrétien Center for Solar System Studies – Palmer Divide Station 446 Sycamore Ave. Table I. List of available telescopes and CCD cameras at CS3. The Eaton, CO 80615 USA exact combination for each telescope/camera pair can vary due to maintenance or specific needs. [email protected] Measurements were made using MPO Canopus. The Comp Star Robert D. Stephens Selector utility in MPO Canopus found up to five comparison Center for Solar System Studies stars of near solar-color for differential photometry. Catalog Landers, CA magnitudes were usually taken from the CMC-15 (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et Daniel R. Coley al., 2009) catalogs. The MPOSC3 catalog was used as a last Center for Solar System Studies resort. The last catalog is based on the 2MASS catalog Landers, CA (http://www.ipac.caltech.edu/2mass) with magnitudes converted (Received: 2016 October 5) from J-K to BVRI (Warner, 2007). The nightly zero points for the catalogs are generally consistent to about ±0.05 mag or better, but Lightcurves for 16 Hilda asteroids were obtained at the on occasion reach 0.1 mag and more. There is a systematic offset Center for Solar System Studies (CS3) from 2016 June among the catalogs so, whenever possible, the same catalog is to September. used throughout the observations for a given asteroid. Period analysis is also done with MPO Canopus, which implements the FALC algorithm developed by Harris (Harris et al., 1989). CCD photometric observations of 16 Hilda asteroids were made at the Center for Solar System Studies (CS3) from 2016 June to In the plots below, the “Reduced Magnitude” is Johnson V as September. This is the first of a planned series on this group of indicated in the Y-axis title. These are values that have been asteroids located between the outer main-belt and Jupiter Trojans. converted from sky magnitudes to unity distance by applying The overall goal is to determine the spin rate statistics of this –5*log (rΔ) to the measured sky magnitudes with r and Δ being, group that has a 3:2 orbital resonance with Jupiter. More respectively, the Sun-asteroid and Earth-asteroid distances in AU. specifically we look to examine the degree of influence that the The magnitudes were normalized to the given phase angle, e.g., YORP effect (Rubincam, 2000) has on more distant objects and to alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is compare the spin rate distribution to the Jupiter Trojans, which can the rotational phase ranging from –0.05 to 1.05. provide evidence that the Hildas are more “comet-like” than main- belt asteroids. If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the amplitude of the Fourier model curve and not necessarily the Table I lists the telescopes and CCD cameras that are combined to adopted amplitude for the lightcurve. The value is meant only to make observations. Up to nine telescopes can be used for the be a quick guide. campaign, although seven is more common. All the cameras use CCD chips from the KAF blue-enhanced family and so have For the sake of brevity, only some of the previously reported essentially the same response. The pixel scales ranged from 1.24- results may be referenced in the discussions on specific asteroids. 1.60 arcsec/pixel. All lightcurve observations were unfiltered since For a more complete listing, the reader is directed to the asteroid a clear filter can result in a 0.1-0.3 magnitude loss. The exposures lightcurve database (LCDB; Warner et al., 2009). The on-line varied depending on the asteroid’s brightness and sky motion. version at http://www.minorplanet.info/lightcurvedatabase.html allows direct queries that can be filtered a number of ways and the results saved to a text file. A set of text files of the main LCDB

Minor Planet Bulletin 44 (2017) 37 tables, including the references with bibcodes, is also available for download. Readers are strongly encouraged to obtain, when possible, the original references listed in the LCDB for their work.

153 Hilda. This 170 km asteroid is the namesake for the Hildas. Shevchenko et al. (2008) found a period of 5.9587 h based on data from several apparitions. Our period spectrum shows a strong solution at 5.954 h, but one at 4.768 h cannot be formally excluded. The two periods differ by almost exactly one rotation over 24 hours. Solutions that differ by integral or half-rotations over the span of the observations are sometimes called rotational aliases because the true number of rotations is not certain.

1269 Rollandia. Franco et al. (2012w) found a period of 15.4 hours with an amplitude of only 0.08 mag. That solution was refined by Fauvaud and Fauvaud (2013), who found 15.32 h based on observations only a few days after the Franco et al. data were obtained in 2012 March.

The CS3 data set was denser than those earlier efforts and did not support the 15.4 h period. Instead the most favored solution in the period spectrum was 19.98 hours, which produced a bimodal lightcurve with an amplitude of 0.06 mag. Since a bimodal solution is not guaranteed with so low an amplitude (Harris et al., 2014), an alternate, monomodal solution at 9.99 hours is also a possibility, especially if the asteroid is nearly spheroidal.

1212 Francette. Taylor et al. (1976) reported only that the period seemed to be longer than 16 h. The CS3 period of 22.433 h is nearly commensurate with an Earth day, which made it difficult to get full coverage of the lightcurve from our single location. 3571 Milanstefanik. There were no previously reported rotation periods in the asteroid lightcurve database (LCDB; Warner et al., 2009). Due to interference from the full Moon, we could not obtain data covering the second maxima. However, the data covered more than one cycle of the adopted period. The estimated damping time from tumbling to single axis rotation for this Minor Planet Bulletin 44 (2017) 38 asteroid exceeds the age of the Solar System (Pravec et al., 2014, and references therein). There were no obvious signs of tumbling, such as the slope of the data for a given night not agreeing with the slope of the Fourier curve. More extensive coverage of the asteroid would be required to determine its true rotational state.

4317 Garibaldi. Dahlgren et al. (1998) observed this Hilda on three nights in 1994. Their phased lightcurve covers only about half their period of 28.5 hours. Our much denser data set spans seven nights. The period spectrum shows the primary and half- period solutions.

3577 Putilin. The period spectrum shows several nearly likely While our data set leads to a strong solution at 7.539 h, this is solutions, including the 29 hours found by Dahlgren et al. (1998) based on the assumption of a typical bimodal lightcurve. Given the and the 18.270 hours found by Brinsfield (2011). Those solutions low amplitude, there is the possibility of a monomodal solution at require unlikely multimodal lightcurves when using the CS3 data, about 3.77 hours. However, the RMS value for the half-period so we adopted a period of 14.30 h for this paper. solution in the period spectrum is significantly larger and we’re confident that the adopted period of 7.539 h is the correct one.

3843 OISCA. De Sanctis et al. (1994) reported finding a period 4446 Carolyn, 8743 Keneke, 11542 Solikamsk, 15278 Paquet, exceeding 16 h. Dahlgren et al. (1998) found a period of 19.078 h (16843) 1997 XX3. There were no previously reported periods in based on sparse data that still produced convincing bimodal the LCDB for these five Hildas. lightcurves. Our observations over ten nights are in good agreement with the Dahlgren results. Given the lightcurve amplitudes, the periods for 4446 Carolyn, 11542 Solikamsk, and 15278 Paquet are considered secure. The low amplitude for 8743 Keneke again raises the possibility of a

Minor Planet Bulletin 44 (2017) 39 solution that has one or three or more maximum/minimum pairs (Harris et al., 2014). A monomodal solution would require a period of only 1.38 hours. Given the diameter of about 28 km, this can be safely ruled out. For (16843) 1997 XX3, the period of 275 h makes it a tumbling candidate and, in fact, there are some sessions where the slope of the data on some nights does not quite correspond with the Fourier curve.

(23974) 1999 CK12. Warner (2012) reported a period of 5.485 h. The latest result of 5.481 h is in good agreement.

17428 Charleroi. There were no previous entries in the LCDB for Charleroi. Here is another example of a low amplitude lightcurve having an unusual, but not necessarily unexpected, shape (see Harris et al., 2014). The unusual features in the lightcurve repeated several times, which gives us full confidence in the derived period of 5.990 h.

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Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. Group 153 Hilda 07/09-07/24 480 13.3,10.5 336 9 5.954 0.002 0.04 0.01 HIL 1212 Francette 07/05-08/02 464 12.9,10.8 165 -3 22.433 0.007 0.13 0.02 HIL 1269 Rollandia 08/08-08/17 432 13.1,12.3 20 -3 19.98 0.02 0.06 0.02 HIL 3571 Milanstefanik 09/01-09/18 1039 5.5,2.6 356 9 421.1 0.6 0.65 0.05 HIL 3577 Putilin 07/14-08/01 319 13.0,10.7 352 4 14.30 0.01 0.11 0.01 HIL 3843 OISCA 08/03-08/12 349 16.1,15.4 19 -1 19.089 0.006 0.32 0.02 HIL 4317 Garibaldi 08/25-08/31 284 6.8,5.5 359 -8 7.539 0.005 0.12 0.02 HIL 4446 Carolyn 07/02-07/17 770 12.0,7.4 310 8 40.92 0.01 0.22 0.02 HIL 8743 Keneke 07/09-07/13 147 13.6,12.9 334 0 2.769 0.002 0.05 0.01 HIL 11542 Solikamsk 08/13-08/19 270 15.6,14.7 15 -1 13.428 0.005 0.49 0.02 HIL 15278 Paquet 09/25-10/02 487 12.9,11.2 40 8 40.01 0.03 0.30 0.02 HIL 16843 1997 XX3 07/14-08/03 444 14.1,9.4 339 1 275 5 0.41 0.04 HIL 17428 Charleroi 09/23-09/28 400 2.7,2.4,2.5 4 9 5.990 0.002 0.12 0.02 HIL 20038 1992 UN5 09/27-10/02 214 15.3,14.2 51 -5 6.944 0.005 0.50 0.02 HIL 32460 2000 SY92 08/25-09/16 1397 10.3,8.4 26 12 49.67 0.03 0.22 0.02 HIL 51874 2001 PZ28 07/06-07/13 206 10.5,12.2 257 13 3.685 0.002 0.19 0.03 HIL

given. LPAB and BPAB are each the average phase angle bisector longitude and latitude (see Harris et al., 1984), unless two values are given (first/last date in range). The Group column gives the orbital group to which the asteroid belongs (all Hildas in this case). The definitions and values are those used in the LCDB (Warner et al., 2009).

(32460) 2000 SY92. This appears to be the first reported period for 2000 SY92. Due to the period being almost commensurate with an Earth day and a full Moon (the bane of asteroid photometry), we were not able to get a complete lightcurve. However, the gap in coverage is relatively small and can be extrapolated without ambiguity and so we consider the period of 49.66 hours to be secure. The period is far short of that required to make the asteroid a candidate for tumbling (Pravec et al., 2014).

(51874) 2001 PZ28. There were no previous entries in the LCDB (20038) 1992 UN5. Polishook (2011) found a period of 6.9 h for for 2001 PZ28, which has an estimated diameter of 13 km. this 27 km Hilda. Our result is consistent with that result.

Minor Planet Bulletin 44 (2017) 41

Closing Remarks de Sanctis, M.C., Barucci, M.A., Angeli, C.A., Fulchignoni, M., Burchi, R., Angelini, P. (1994) “Photoelectric and CCD The additional results from this paper bring to 106 the number of observations of 10 asteroids.” Plan. Space Sci. 42 859-864. Hilda asteroids with statistically useful periods (see Warner et al., 2009). These are shown as yellow (light) circles in the frequency- Fauvaud, S., Fauvaud, M. (2013). “Photometry of Minor Planets. diameter plot from the LCDB as of 2016 October 4. I. Rotation Periods from Lightcurve Analysis for Seven Main-belt Asteroids.” Minor Planet Bul. 40, 224-229.

Franco, L., Zambelli, R. (2012w). http://digilander.libero.it/ A81_Observatory

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics

on an asteroid lightcurve.” Icarus 235, 55-59. Of particular note is the number Hildas with D < 15 km, which account for about 27% of the total of 106. These will be more Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, likely subject to thermal forces such as YORP. Since the Hildas T.C., Welch, D.L. (2009). http://www.aavso.org/apass tend to be lower albedo (p ~ 0.05), it will be a challenge to extend V Pravec, P., Scheirich, P., Durech, J., Pollock, J., Kusnirak, P., the rotation statistics to smaller members of the orbital group. Hornoch, K., Galad, A., Vokrouhlicky, D., Harris, A.W., Jehin, E., With a 0.75-meter telescope to come on-line in the near future at Manfroid, J., Opitom, C., Gillon, M., Colas, F., Oey, J., Vrastil, J., CS3, we believe we’ll be able to add a significant number of Reichart, D., Ivarsen, K., Haislip, J., LaCluyze, A. (2014). “The rotation periods for the smaller Hildas. tumbling state of (99942) Apophis.” Icarus 233, 48-60. Acknowledgements Polishook, D. (2011). “Lightcurves and Spin Periods from the Funding for PDS observations, analysis, and publication was Wise Observatory – 2010.” Minor Planet Bul. 38, 18-21. provided by NASA grant NNX13AP56G. Work on the asteroid Shevchenko, V.G., Tungalag, N., Chiorny, V.G., Gaftonyuk, lightcurve database (LCDB) was also funded in part by National N.M., Krugly, Yu.N., Harris, A.W., Young, J.W. (2009). CCD- Science Foundation grant AST-1507535. photometry and pole coordinates for eight asteroids.” Plan. Space This research was made possible in part based on data from Sci. 57, 1514-1520. CMC15 Data Access Service at CAB (INTA-CSIC) Rubincam, D.P. (2000). “Relative Spin-up and Spin-down of (http://svo2.cab.inta-csic.es/vocats/cmc15/) and the AAVSO Small Asteroids.” Icarus 148, 2-11. Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. Taylor, R.C., Gehrels, T., Capen, R.C. (1976). “Minor planets and related objects. XXI - Photometry of eight asteroids.” Ap. J. 81, This publication makes use of data products from the Two Micron 778-786. All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Warner, B.D. (2007). “Initial Results of a Dedicated H-G Center/California Institute of Technology, funded by the National Program.” Minor Planet Bul. 34, 113-119. Aeronautics and Space Administration and the National Science Foundation. (http://www.ipac.caltech.edu/2mass/) Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2016 July. References http://www.minorplanet.info/lightcurvedatabase.html

Brinsfield, J.W. (2011). “Asteroid Lightcurve Analysis at the Via Warner, B.D. (2012). “Asteroid Lightcurve Analysis at the Palmer Capote Observatory: 1st Quarter 2011.” Minor Planet Bul. 38, Divide Observatory: 2011 December - 2012 March.” Minor Planet 154-155. Bul. 39, 158-167. Dahlgren, M., Lahulla, J.F., Lagerkvist, C.-I., Lagerros, J., Mottola, S., Erikson, A., Gonano-Beurer, M., Di Martino, M., (1998). “A Study of Hilda Asteroids. V. Lightcurves of 47 Hilda Asteroids.” Icarus 133, 247-285.

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MAIN-BELT ASTEROID LIGHTCURVES FROM magnitudes > 18, night-to-night calibration of the data (generally CERRO TOLOLO INTER-AMERICAN OBSERVATORY – < ±0.05 mag) was mostly done using the CMC-14 catalog. Some 2016 APRIL comparison stars were measured using the MPOSC3 catalog provided with Canopus, whose stars are converted to approximate Robert D. Stephens Cousins R magnitudes based on 2MASS J-K colors (Warner Center for Solar System Studies (CS3)/MoreData! 2007). 11355 Mount Johnson Ct., Rancho Cucamonga, CA 91737 USA [email protected] In the lightcurve plots, the “Reduced Magnitude” is Johnson R corrected to a unity distance by applying -5*log (r∆) to the Linda M. French measured sky magnitudes with r and ∆ being, respectively, the Illinois Wesleyan University Sun-asteroid and the Earth-asteroid distances in AU. The Bloomington, IL USA magnitudes were normalized to the phase angle given in parentheses using G = 0.15. David James Cerro Tololo Inter-American Observatory With the exception of 22550 Jonsellon and (211523) 2003 QX60, La Serena, Chile none of these asteroids had previously reported rotational periods in the Lightcurve Database (LCDB; Warner et al., 2009). Derrick Rohl Adventure Science Center (12676) 1981 DU1. Due to having only 55 data points over two Nashville, TN USA nights, competing periods exist near 7 and 14 h as shown by the period spectrum. We prefer the 10.21 h period because it has the Brian D. Warner best bimodal symmetrical lightcurve. Center for Solar System Studies / MoreData! Inc. Eaton, CO USA (20906) 2727 P-L. Because the period is close to one-half the Earth’s rotation, we could not get a complete lightcurve over two (Received: 2016 October 6) consecutive nights. However, the large amplitude leaves little doubt the period is near 12 h. Thirty main-belt asteroids were observed from CTIO (Cerro Tololo Inter-American Observatory MPC 807) in 22550 Jonsellon. This inner main-belt asteroid was on the DECam April 2016. Rotational periods were determined for 25 chips for only a single night, not ‘minding the gap’ on the first of them. Four are reported as having an indeterminate night of clear weather. Still, this result is near the result found by long-period. Waszczak et al. (2015) who used sparse data from the Palomar Transit Factory Survey to report a period of 2.6424 h. Harris et al (2014) and Warner et al (2011) showed that sparse photometric Observations of 30 main-belt asteroids were obtained as a data has a distinct bias against finding short rotational periods, but byproduct of an observing run targeting Jovian Trojans. Observing the combination of the two results lends confidence of the time was scheduled for five nights on the 4-Meter Victor Blanco determination. telescope at CTIO. Two fields were observed in the heart of the Trojan cloud and followed for up to six hours each clear night. (34742) 2001 QD79. The period spectrum showed several aliases Clouds compromised most of the nights during the five night run. near 7, 9, 10 and 14 h. We prefer the 8.81 h solution because it Three nights were completely lost, one half night had the data produced a symmetrical, bimodal lightcurve. degraded due to bad seeing because the air conditioning system keeping the mirror cool during the day failed, and the final night (37801) 1997 WO47. From the slope of this high-amplitude lost the last hour of observing from passing high cirrus clouds. lightcurve, it is apparent that the rotational period exceeds 24 h. Given only partial data from two nights, we would not normally The observing strategy was designed to provide the greatest think that a period could be estimated. However, we were able to chance to derive rotational periods for the Trojan asteroids, which plot what looks to be a reasonable half period of 18.75 h. If worked equally well for the main-belt asteroids found in the same correct, one could expect a complete rotational period to be near fields. The main difference was that the main-belt asteroids were 37.5 h. moving twice as fast as the Trojans, tended to move across chips quicker, and sometimes moved entirely out of the field of view. (45209) 1999 XT178. Like (20906) 2727 P-L, this inner main-belt The Moon was nearly full and close to the L4 Trojan cloud during asteroid appears to have a rotational period near one-half the the observing run. Therefore, fields were selected where the Moon Earth’s rotation. The period spectrum does not show any close was at least 20 degrees away. aliases and the data collected are consistent with a normal bimodal lightcurve. The images were obtained using the 4-meter Blanco telescope and the Dark Energy Camera (DECam). Exposures were 300 seconds (61652) 2000 QO112. The data collected favor a low-amplitude through the DECam r filter. Even with the shortened two night bimodal lightcurve with a few outliers on the first night which had observing run, it would be possible to estimate or determine poor seeing over the first half. However, with an amplitude of rotational periods for most asteroids with a period up to a day in around 0.07 magnitudes, it is possible that the lightcurve could length. However, the longer the rotational period, the more under- have only a single extremum, or three or more extrema (Harris et sampled it would be and so reduce the confidence in the result. al 2014).

Image processing, measurement and period analysis was done (66889) 1999 VW78. As with the previously discussed lightcurve, using MPO Canopus (Bdw Publishing), which incorporates the this outer main-belt asteroid has an amplitude of 0.07 magnitudes. Fourier analysis algorithm (FALC) developed by Harris (Harris et Therefore, it is possible this one could not be a bimodal lightcurve. al., 1989). Because there are no reliable star catalogs with The period spectrum shows an alias near 7 h. Minor Planet Bulletin 44 (2017) 43

Number Name 2016 mm\dd Pt Phase LPAB BPAB Period P.E. Amp A.E. Grp 12676 1981 DU1 04/26-04/27 55s 3.1,2.8 224 -3 10.21 0.05 0.14 0.02 MB-O 14256 2000 AA96 04/26-04/27 71 2.6,2.2 223 -1 >96 >.70 MB-O 20163 1996 UG 04/26-04/27 60 2.7,2.3 222 -1 5.08 0.01 0.14 0.02 MB-I 20906 2727 P-L 04/26-04/27 72 4.8,4.3 223 -3 11.57 0.04 0.68 0.05 FLOR 22550 Jonsellon 04/27-04/27 37 15.4,15.4 354 5 2.8 0.01 0.21 0.02 MB-I 30251 Ashkin 04/26-04/27 64 2.6,2.1 222 -1 5.6 0.01 0.74 0.05 MB-I 34742 2001 QD79 04/26-04/27 62 2.6,2.2 222 -1 8.81 0.02 0.3 0.02 MB-M 37801 1997 WO47 04/26-04/27 68 3.8,3.3 223 -3 37.5 0.25 > 1. FLOR 43692 2160 P-L 04/26-04/27 62 3.3,2.8 223 0 3.46 0.01 0.16 0.02 FLOR 43956 Elidoro 04/26-04/27 58 4.5,4.0 224 -3 >24 MB-I 45209 1999 XT178 04/26-04/27 54 3.0,2.6 223 -1 11.9 0.1 0.19 0.05 MB-I 61652 2000 QO112 04/26-04/27 68 3.1,2.7 223 0 3.367 0.015 0.07 0.02 MB-M 64787 2001 XH200 04/26-04/27 39 3.5,3.0 223 0 2.84 0.01 0.3 0.03 MB-M 66889 1999 VW78 04/26-04/27 55 3.1,2.6 223 -1 10.7 0.2 0.07 0.02 MB-O 71933 2000 WW61 04/26-04/27 44 2.8,2.3 222 -1 3.37 0.01 0.11 0.02 MB-I 73987 1998 EA2 04/26-04/26 54 4.9,4.9 224 -3 >72 FLOR 80940 2000 DD86 04/26-04/27 56 4.5,4.0 224 -3 3.48 0.01 0.36 0.03 V 91040 1998 FD14 04/26-04/27 79 2.8,2.4 223 0 4.62 0.02 0.13 0.02 MB-M 107924 2001 FO103 04/26-04/27 71 4.8,4.3 223 -3 3.599 0.003 0.48 0.02 MB-I 110572 2001 TH115 04/26-04/27 55 3.3,2.9 224 -3 3.19 0.01 0.16 0.03 MB-M 117687 2005 EX259 04/26-04/27 51 3.8,3.2 222 0 15.47 0.13 0.18 0.03 MB-I 122092 2000 HZ50 04/26-04/27 50 4.3,3.6 222 -1 FLOR 125268 2001 VJ2 04/26-04/27 61 3.7,3.2 223 0 >24 FLOR 125979 2001 YU21 04/26-04/27 59 4.1,3.5 222 0 5.29 0.02 0.67 0.03 FLOR 127288 2002 JV74 04/26-04/27 78 3.2,2.7 222 -1 10.3 0.02 0.33 0.03 MB-O 211523 2003 QX60 04/26-04/27 67 3.5,2.9 222 -1 6.54 0.01 0.54 0.03 FLOR 221794 2008 BC34 04/26-04/27 54 3.9,3.3 222 0 11.39 0.06 0.8 0.05 NYSA 228653 2002 EZ129 04/26-04/27 45 3.1,2.6 223 0 8.29 0.04 0.23 0.03 MB-O 375941 2009 WE102 04/26-04/27 58 4.1,3.6 223 -1 3.64 0.01 0.12 0.02 MB-I 376052 2010 EH44 04/26-04/27 73 2.6,2.2 222 0 > 80 < 1 MB-O Table I. Observing circumstances. Pts is the number of data points used in the analysis. The phase angle (α) is given at the start and end of each date range, unless it reaches a minimum, which is then the second of the three values. LPAB and BPAB are, respectively the average phase angle bisector longitude and latitude. Grp is the asteroid family.

(110572) 2001 TH115. The period spectrum shows an alias near Foundation. This research was supported by National Science 6 h, but we prefer the 3.19 h solution because it produces a Foundation grant AST-1212115. bimodal solution. References (117687) 2005 EX259. The period spectrum shows several aliases near 8, 10, 15 and 24 h. To break the tie, we plotted the lightcurve Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., for a half period solution of 7.63 creating a single modal Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, lightcurve. While Harris et al (2014) shows that a single modal H., Zeigler, K.W. (1989). “Photoelectric Observations of lightcurve with an amplitude of 0.17 mag to be possible, a Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. bimodal solution twice that at 15.47 h is more likely and is the period we are adopting. Harris, A.W., Pravec, P., Galád, B. Skiff, B., Warner, B., Világi, J., Gajdoš, S., Carbognani, A., Hornoch, K., Kušnirák, P., Cooney, (221794) 2008 BC34. This is another case where the high- W., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B. amplitude lightcurve produces a rotational period near half the (2014). “On the maximum amplitude of harmonics of an asteroid Earth’s rotation. Plotting for the half-period of 5.67 h shows the lightcurve.” Icarus 235, 55-59. likely rotational period to be 11.39h. Harris, A.W., Warner, B.D., Pravec, P. (2014). “Looking a gift (228653) 2002 EZ129. The period spectrum shows strong aliases horse in the mouth: Evaluation of wide-field asteroid photometry near 2.6, 5, 8 and 10 h. The strongest alias at just over five hours surveys.” Icarus 221, 226-235. produces an unlikely single modal lightcurve with a 0.18 amplitude magnitude. We prefer the 8.29 h bimodal solution. Warner, B.D. (2007). “Initial Results from a Dedicated H-G Project.” Minor Planet Bul. 34, 113-119. Acknowledgements Warner, B.D., Harris, A.W. (2011). “Using sparse photometric French and Stephens were visiting astronomers at Cerro Tololo data for asteroid lightcurve studies.” Icarus 216, 610-624. Inter-American Observatory, National Optical Astronomy Observatory, operated by the Association of Universities for Warner, B.D., Harris, A.W., Pravec, P. (2009). Icarus 202, 134- Research in Astronomy, under contract with the National Science 146. Updated 2016 September 09. http://www.minorplanet.info/lightcurvedatabase.html.

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Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry.” Ap. J. 150, A75.

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ASTEROIDS OBSERVED FROM CS3: 2016 JULY - SEPTEMBER

Robert D. Stephens Center for Solar System Studies (CS3)/MoreData! 11355 Mount Johnson Ct., Rancho Cucamonga, CA 91737 USA [email protected]

(Received: 2016 October 6)

CCD photometric observations of twelve asteroids were obtained at the Center for Solar System Studies from 2016 July to September.

The Center for Solar System Studies “Trojan Station” (CS3, MPC U81) has two telescopes which are normally used in program asteroid family studies. Those targets are usually too dim to continue observations during bright moon times, so these brighter targets, suitable for future shape modeling studies, were selected to keep the telescopes operating.

All images were made with a 0.4-m or a 0.35-m SCT using an FLI ML-Proline 1001E or FLI ML-Microline 1001E CCD camera. Images were unbinned with no filter and had master flats and darks applied. Image processing, measurement, and period analysis were done using MPO Canopus (Bdw Publishing), which incorporates the Fourier analysis algorithm (FALC) developed by Harris (Harris et al., 1989). Night-to-night calibration of the data (generally < ±0.05 mag) was done using field stars converted to approximate Cousins V magnitudes based on 2MASS J-K colors (Warner 2007a). The Comp Star Selector feature in MPO Canopus was used to limit the comparison stars to near solar color.

In the lightcurve plots, the “Reduced Magnitude” is Johnson V corrected to a unity distance by applying -5*log (r∆) to the measured sky magnitudes with r and ∆ being, respectively, the Sun-asteroid and the Earth-asteroid distances in AU. The magnitudes were normalized to the phase angle given in parentheses using G = 0.15.

1293 Sonja. This Mars-crosser has being well studied over the years. Higgins et al (2007), Behrend (2006), Benishek (2008), and Parvec et al (2016) each found rotational periods near 2.88 h. The result found this year is in agreement with those findings.

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. Grp 1293 Sonja 07/16-07/18 188 15.1,14.2 310 8 2.879 0.001 0.17 0.01 MC 2233 Kuznetsov 08/21-08/24 216 5.8,4.5 337 5 5.031 0.002 0.23 0.02 FLOR 2272 Montezuma 09/17-09/24 120 26.7,28.0 309 18 8.182 0.001 1.53 0.02 H 4132 Bartok 07/24-07/26 162 16.1,15.5 331 15 3.298 0.001 0.44 0.02 PHO 8783 Gopasyuk 08/21-08/24 196 2.6,2.5,2.6 330 5 5.693 0.002 0.63 0.02 V 16585 1992 QR 07/29-08/05 190 27.6,25.3 348 -3 5.25 0.003 0.20 0.02 H 19300 1996 SH6 07/11-07/28 310 12.2,18.1 271 11 17.14 0.01 0.24 0.05 V 30019 2000 DD 09/15-09/17 152 22.3,21.3 25 2 5.55 0.01 0.16 0.03 H 30958 1994 TV3 08/18-08/20 95 27.4,26.8 9 10 5.78 0.01 0.67 0.03 H 46818 1998 MZ24 07/18-07/20 90 14.7,15.3 293 20 2.78 0.01 0.20 0.03 PHO 102912 1999 XA21 07/21-07/28 270 28.5,27.8 313 36 41.6 0.1 0.78 0.05 MC 163694 2003 DP13 07/29-08/01 106 23.9,21.6 334 -1 2.387 0.002 0.13 0.02 NEA Table I. Observing circumstances. Pts is the number of data points used in the analysis. The phase angle (α) is given at the start and end of each date range, unless it reaches a minimum, which is then the second of the three values. LPAB and BPAB are, respectively the average phase angle bisector longitude and latitude. Grp is the asteroid group/family (Warner et al., 2009). Minor Planet Bulletin 44 (2017) 50

2233 Kuznetsov. Ditteon et al (2011) found a rotational period of 8783 Gopasyuk. The rotational period for this Vestoid was 5.030 h. The latest result agrees with those 2011 observations. determined twice in the past with sparse photometry from surveys. Using data from the Thousand Asteroid Light Curve Survey, Masiero et al (2009) found a period of 5.6951 h. Using data from the Palomar Transient Factory, Waszczak et al. (2015) reported a period of 5.6933 h. Our dense lightcurve this year confirms the results from these sparse data surveys.

2272 Montezuma. We have studied this Hungaria twice in the past as part of a Hungaria family pole position study. Warner (2012a) found a rotational period of 8.183 h and the author (Stephens et al 2014) found a period of 8.180 h. Our result this year is in agreement with our prior findings and helped refine the sidereal period to be 8.18880501 h. (16585) 1992 QR. Warner (2007b, 2012c, and 2015) studied this asteroid three times before as a part of a study of Hungaria family members pole solutions, each time reporting periods near this result of 5.25 h

4132 Bartok. Rotational periods for this asteroid have been determined three times in the past. Skiff observed it in 2011, finding a period of 3.297 h. Warner (2014) and Behrend (2014) also observed it, finding periods of 3.297 h. The result found this year agrees with those prior findings.

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(19300) 1996 SH6. There were no previously reported rotation (46818) 1998 MZ24. Warner (2010) previously observed this periods of this Vestoid in the asteroid lightcurve database (LCDB; asteroid, finding a rotational period of 2.779 h. This result agrees Warner et al., 2009). with the previous finding.

(30019) 2000 DD. Warner (2012b) observed this Hungaria family (102912) 1999 XA21. There were no previously reported rotation member twice before in 2006 and 2011. Skiff observed it once in periods of this Mars-crosser in the asteroid lightcurve database 2011. Both reported a rotational period near 5.49 h, close to the (LCDB; Warner et al., 2009). result found this year.

(163694) 2003 DP13. There were no previously reported rotation (30958) 1994 TV3. Warner (2014) observed this Hungaria in 2013 periods of this Near-Earth asteroid in the asteroid lightcurve reporting a rotational period of 5.811 h, similar to the result found database (LCDB; Warner et al., 2009). With a rotational period this year. close to the ‘spin-barrier’ there is a possibility this asteroid could be a binary. However, the data obtained were not of sufficient quality to reveal attenuation events.

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Acknowledgements Warner, B.D. (2015). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2014 December - 2015 March.” Minor Planet This research was supported by NASA grant NNX13AP56G. Bul. 42, 167-172.

The purchase of a FLI-1001E CCD cameras was made possible by Warner, B.D., Harris, A.W., Pravec, P. (2009). Icarus 202, 134- a 2013 Gene Shoemaker NEO Grants from the Planetary Society. 146. Updated 2016 September 09. http://www.minorplanet.info/lightcurvedatabase.html. References Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., Behrend, R. (2016). Observatoire de Geneve web site, Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., http://obswww.unige.ch/~behrend/page_cou.html. Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Benishek, V. (2008). “CCD Photometry of Seven Asteroids at the Periods and Phase Functions from Sparse Photometry.” Ap. J. 150, Belgrade Astronomical Observatory.” Minor Planet Bul. 35, 28- A75. 30.

Ditteon, R., West, J. (2011). “Asteroid Lightcurve Analysis at the Oakley Southern Observatory: 2011 January thru April.” Minor ASTEROIDS LIGHTCURVES ANALYSIS AT OAVDA: Planet Bul. 38, 214-217. 2016 JANUARY – OCTOBER

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Albino Carbognani Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Astronomical Observatory of the H., Zeigler, K.W. (1989). “Photoelectric Observations of Aosta Valley Autonomous Region (OAVdA) Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Lignan 39, 11020 Nus (Aosta), ITALY [email protected] Higgins, D., Goncalves, R. (2007). “Asteroid Lightcurve Analysis at Hunters Hill Observatory and Collaborating Stations - June- (Received: 2016 Oct 13 Revised: 2016 Nov 14) September 2006.” Minor Planet Bul. 34, 16-18. Ten main-belt and near-Earth asteroids were observed Masiero, J., Jedicke, R., Durech, J., Gwyn, S., Denneau, L., from 2016 January-October to find the synodic rotation Larsen, J. (2009). “The Thousand Asteroid Light Curve Survey.” period and lightcurve amplitudes for each asteroid. Icarus 204, 145-171. Results are reported for 1770 Schlesinger, 3433 Fehrenbach, 3792 Preston, (7350) 1993 VA, (10150) Parvec, P. (2016). Photometric Survey for Asynchronous Binary 1994 PN, (357024) 1999 YR14, (458198) 2010 RT11, Asteroids web site. http://www.asu.cas.cz/~asteroid/binast (471241) 2011 BX18, 480004 (2014 KD91), and 2016 photsurvey.htm. LX48. Stephens, R.D., Coley, D., Warner, B.D. (2014). “Collaborative Asteroid Lightcurve Analysis at the Center for Solar System This paper features the results of photometric observations of Studies: 2013 April-June.” Minor Planet Bul. 41, 8-13. main-belt (MBA) and near-Earth (NEA) asteroids made at OAVdA (Carbognani et al., 2007) from 2016 Jan to Oct. We Warner, B.D. (2007a). “Initial Results from a Dedicated H-G observes the MBAs in collaboration with the Photometric Survey Project.” Minor Planet Bul. 34, 113-119. for Asynchronous Binary Asteroids (Pravec, 2005) when there is Warner, B.D. (2007b). “Asteroid Lightcurve Analysis at the some interesting target (i.e., a suspected binary asteroid). Work on Palmer Divide Observatory - December 2006 - March 2007.” NEAs is done when the rotation periods were not known (or at Minor Planet Bul. 34, 72-77. least uncertain) at the time of observations. The observing circumstances and results are given in Table I. Warner, B.D. (2010). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2009 June-September.” Minor Planet Bul. Until 2016 September 19, images at OAVdA were captured with a 37, 24-27. modified Ritchey-Chrétien f/7.9 0.81-m telescope and FLI 1001E CCD camera with an array of 1024×1024 pixels. The field-of- Warner, B.D. (2012a). “Asteroid Lightcurve Analysis at the view was 13.1×13.1 arcmin and the plate scale was Palmer Divide Observatory: 2011 June - September.” Minor 1.54 arcsec/pixel in 2x2 binning mode. Afterwards, a focal Planet Bul. 39, 16-21. reducer, funded by a 2013 Shoemaker NEO Grant, was installed. This reduced the focal ratio to f/4.7. This increased the field-of- Warner, B.D. (2012b). “Asteroid Lightcurve Analysis at the view to 22.5×22.5 arcmin and the plate scale to 2.64 arcsec/pixel Palmer Divide Observatory: 2011 September - December.” Minor in 2x2 binning mode. Considering that the full width at half Planet Bul. 39, 69-80. maximum (FWHM) of the stars 45° above the horizon from Warner, B.D. (2012c). “Asteroid Lightcurve Analysis at the OAVdA is about 4.8-5.0 arcsec, the 2x2 binning mode appears to Palmer Divide Observatory: 2011 December - 2012 March.” be the best for photometry. Minor Planet Bul. 39, 158-167. MPO Canopus (Warner, 2009a) version 10.7.1.3 was used for Warner, B.D. (2014). “Asteroid Lightcurve Analysis at CS3- differential photometry and period analysis. When possible, the Palmer Divide Station: 2013 June - September.” Minor Planet sessions were calibrated with the MPO Canopus Comp Star Bul. 41, 27-32. Selector (CSS), which chooses comparison stars that are similar in

Minor Planet Bulletin 44 (2017) 53 color to the target (in general solar-type stars), and the DerivedMags approach.

1770 Schlesinger is an MBA. A total of 354 images were taken with a clear filter and 120 s exposures on three nights: 2016 Mar 10-11 and 21. The data from the last session were affected by moonlight. Magnitudes for the comparison stars were taken from the MPOSC3 catalog (see Warner, 2007). The result of the data analysis gave a period of 2.881 ± 0.001 h and amplitude of 0.31 mag. The period is in good agreement with that reported in the asteroid lightcurve database (LCDB; Warner et al., 2009b).

3792 Preston is an MBA. A total of 119 images were taken with an R filter on 2016 March 18. Comparison star magnitudes were taken from the MPOSC3 catalog. Data analysis found a period of 2.947 ± 0.014 h and amplitude of 0.27 mag. This period is in good agreement with the LCDB summary line value.

3433 Fehrenbach is an MBA. A total of 131 images were taken with a clear filter and exposures of 120 s on 2016 Jan 29. Comparison star magnitudes were taken from the MPOSC3 catalog. Data analysis found a period of 3.907 ± 0.014 h and amplitude of 0.34 mag. The rotation period is in good agreement with that reported in LCDB.

(7350) 1993 VA is an Apollo object which made an Earth flyby on 2016 Mar 23 at 0.153 AU. A total of 578 images using a clear filter and exposures of 60-180 s were taken in three nights in April and two in May. MPOSC3 magnitudes were used for the comparison stars. Data analysis found a bimodal lightcurve with a period of 3.584 ± 0.002 h and amplitude of 0.26 mag. In the last three sessions, the lightcurve was not fully covered and the

Minor Planet Bulletin 44 (2017) 54 amplitude dropped to 0.19 mag. The period, unknown at the time of our observations, is in good agreement with Warner (2016a).

(357024) 1999YR14 is an Apollo object, classified as a potentially hazardous asteroid (PHA), which made an Earth flyby on 2016 September 1 at 0.056 AU. This asteroid was observed on September 7 and 8. A total of 437 images using a clear filter and exposures of 30 s were taken. The CMC15 catalog was used for comparison star magnitudes. The rotation period, unknown at the time of our observations, was found to be 4.246 ± 0.002 h with an amplitude of about 1.38 mag. The lightcurve appears symmetrical and the large amplitude is indicative of an elongated asteroid.

(10150) 1994 PN is an Amor asteroid. A total of 107 images were taken with a clear filter and 120 s exposures on 2016 Jul 5 and 6. The first session was short (about 1 h), while the second was a bit longer (about 2.3 h). Both used CMC15 magnitudes for the comparison stars. The result is a complex lightcurve with a period of 2.632 ± 0.003 h and amplitude of 0.24 mag. According to Warner (2016b), this asteroid may be binary. These new data are not sufficient to support this hypothesis.

(458198) 2010 RT11 is an Amor object (0.4-1.2 km diameter), which made an apparition on 2016 May 21 at 0.25 AU. A total of 104 images were taken with a clear filter and 180 s exposures on 2016 May 26 and Jun 09. Comparison star magnitudes used, Minor Planet Bulletin 44 (2017) 55 respectively, the MPOSC3 and CMC15 stars catalogs. In the first session (3 hours long), the lightcurve showed a complex shape with 3 maxima and minima and a possible rotation period of 1.754 ± 0.038 h with an amplitude of 0.15 mag. In the period spectrum there is also a secondary minimum corresponding about to the half of this period. The period is interesting given the estimated diameter because it is faster than the so-called spin-barrier at about 2.2 h (Pravec, 2002). In the second session (2 hours long), the asteroid was in a very crowded star field and so data when the asteroid was close to a star were excluded from the analysis. This caused a gap of about 1 h. It was not possible to establish a rotation period from this session. Moreover, the amplitude increased to 0.22 mag, making it difficult to merge the two lightcurves to refine the period. This asteroid could be a large super-fast rotator but the case remains very ambiguous and more data are needed. No period was known for this object before.

480004 (2014 KD91) is an Amor asteroid that made an Earth flyby on 2016 Oct 25 at 0.22 AU. It was observed before closest approach on Sep 28 and Oct 3-5. Overall, a total of 516 images with clear filter and exposures of 120 s were taken. Photometry was difficult because the asteroid moved in very crowded star fields. The lightcurve appears almost bimodal, with a rotation period of 2.837 ± 0.001 h and amplitude of 0.18 mag. No period was known for this object before.

(471241) 2011 BX18 is an Apollo object classified as a PHA. It had an apparition on 2016 Jul 25 at 0.135 AU. A total of 469 images with clear filter and exposures of 60 s were taken on 2016 Aug 6 and 8. The total observing time was about 8 hours. Due to the rapid sky motion of 5.6 arcsec/min, each night was divided into two parts. CMC15 magnitudes were used for the comparison stars. The resulting lightcurve is noisy and complex but the most probable rotation period is 3.448 ± 0.002 h with an amplitude of 0.32 mag. However, additional higher quality data will be necessary to confirm this result.

Minor Planet Bulletin 44 (2017) 56

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. 1770 Schlesinger 03/10-03/21 354 20.7,22.7 122 6 2.881 0.001 0.31 0.02 3433 Fehrenbach 01/29 131 26.6 75 5 3.907 0.014 0.34 0.02 3792 Preston 03/18 119 25.0 152 33 2.947 0.014 0.27 0.02 7350 1993 VA 04/06-05/04 578 62.4,42.6 178 21 3.587 0.002 0.26 0.02 10150 1994 PN 07/05-07/06 107 32.4 262 34 2.632 0.003 0.24 0.02 357024 1999 YR14 09/07-09/08 437 79.7,81.8 333 28 4.246 0.002 1.38 0.02 458198 2010 RT11 05/26-06/09 104 4.4,11.1 246 3 1.75 0.04 0.15 0.02 471241 2011 BX18 08/06-08/08 469 70.9,64.9 356 14 3.448 0.002 0.32 0.02 2014 KD91 09/28-10/05 516 24.7,18.5 127 -5 2.837 0.001 0.18 0.02 2016 LX48 09/06-09/08 644 92.0,86.4 298 18 3.815 0.001 0.55 0.02

2016 LX48 is an Apollo object classified as a PHA, discovered by Acknowledgements Pan-STARRS I on 2016 Jun 11. It made an Earth flyby on 2016 Sep 12 at 0.045 AU. A total of 644 images with clear filter and This research made use of the NASA’s Astrophysics Data System exposures of 30 s were taken on the nights of Sep 6-8. As with and JPL’s Small-Body Database Browser. Research at the 2010 RT11, photometry was difficult because the asteroid moved Astronomical Observatory of the Aosta Valley Autonomous in very crowded star fields. The lightcurve appears bimodal with a Region was supported by the 2013 Shoemaker NEO Grant. rotation period of 3.815 ± 0.001 h with amplitude 0.55 mag. However, the coverage is not complete and the true value of the References rotation period may be different. This asteroid was also a radar target for Arecibo on Sep 9-11. The Arecibo team found an Carbognani, A., Calcidese, P. (2007). “Lightcurve and Rotational elongated shape with dimension of 0.7x1.0 km. In order for the Period of Asteroids 1456 Saldanha, 2294 Andronikov and 2006 period to match the optically-derived period with the radar-derived NM.” Minor Planet Bulletin 34, 18-19. period, 2016 LX48 had to be seen from a sub-radar latitude of Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). about 50°-60°. No period was known for this object before. “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Pravec, P., Harris, A.W., and Michalowski, T. (2002). “Asteroid Rotations”. Asteroids III (W. Bottke, A. Cellino, P. Paolicchi, R. P. Binzel, eds), University of Arizona Press, Tucson.

Pravec, P. (2005). “Photometric Survey for Asynchronous Binary Asteroids”, The Society for Astronomical Sciences, 24, 61-67.

Warner, B.D. (2007). “Initial Results of a Dedicated H-G Program.” Minor Planet Bul. 34, 113-119.

Warner, B.D. (2009a). MPO Software, MPO Canopus. Bdw Publishing. http://minorplanetobserver.com/

Warner, B.D., Harris, A.W, Pravec, P. (2009b). “The asteroid Lightcurve Database.” Icarus 202, 134-146. Revision consulted: http://www.minorplanet.info/datazips/LCLIST_PUB_2016SEP.zip

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Warner, B.D. (2016a). “Near-Earth Asteroid Lightcurve Analysis Warner, B.D. (2016b). “Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2016 January – April.” Minor at CS3-Palmer Divide Station: 2016 April – July.” Minor Planet Planet Bul. 43, 240-250. Bul. 43, 311-319.

ASTEROID LIGHTCURVE ANALYSIS AT ASTRONOMICAL OBSERVATORY – UNIVERSITY OF SIENA (ITALY): 2016 MAY-SEPTEMBER

Fabio Salvaggio Gruppo Astrofili Catanesi 21047 – Saronno, ITALY [email protected]

Alessandro Marchini Astronomical Observatory, DSFTA - University of Siena (K54) via Roma, 56, 53100 – Siena, ITALY

Riccardo Papini Carpione Observatory (K49) San Casciano in Val di Pesa (FI), ITALY

(Received: 2016 October 13) From 2016 May to September, CCD images were taken 3743 Pauljaniczek is a main-belt asteroid discovered in 1983 with the goal of analyzing the photometric data and March by Ewan Barr. Its orbit has a semi-major axis of about calculating the rotation period of six asteroids: 2.202 AU, eccentricity 0.148, and period of about 3.27 years. We 3008 Nojiri, 3743 Pauljaniczek, 3925 Tret’yakov, observed this asteroid from 2016 May 27 to June 14. The (11250) 1972 AU, (19516) 1998 QF80, and 23587 collaborative observations resulted in five sessions. The result for Abukumado. a bimodal lightcurve is a synodic period of 4.558 ± 0.001 h with an amplitude of 0.27 ± 0.03 mag.

Lightcurve analysis was performed using images taken at the Astronomical Observatory of the University of Siena (Italy). The equipment used to obtain the images were a 0.30-m f/5.6 Maksutov-Cassegrain, SBIG STL-6303E NABG CCD camera, and clear filter; the pixel scale was 2.26 arcsec/pix with 2x2 binning. Exposures were 300 seconds. The images were calibrated using Maxim DL software. MPO Canopus (Warner, 2013) was used to measure the images, do Fourier analysis, and produce the lightcurves. Table I gives the observing circumstances and results for each asteroid.

Orbital data and discovery circumstances were taken from the JPL Small Bodies Node (JPL, 2016).

3008 Nojiri is a main-belt asteroid discovered on 1938 November 17 by K. Reinmuth. Its orbit has a semi-major axis of about 3.17 AU, eccentricity 0.129, and period of about 5.67 years. We observed this asteroid from 2016 September 24-26. The collaborative observations resulted in three sessions. Our result for a bimodal lightcurve is a synodic period of 5.855 ± 0.004 h and 3925 Tret’yakov is a main-belt asteroid discovered on 1977 amplitude of 0.42 ± 0.04 mag. September 19 by L. Zhuravleva. Its orbit has a semi-major axis of about 2.397 AU, eccentricity 0.194, and period of about 5.61

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. Grp 3008 Nojiri 09/24-09/26 198 16.2,17.3 349 0 5.855 0.004 0.42 0.05 THM 3743 Pauljaniczek 05/29-06/14 151 25.7 264 4 4.558 0.001 0.27 0.02 FLOR 3925 Tret’yakov 08/03-09/23 520 1.4,2.3 335 3 30.962 0.002 0.24 0.03 MB-O 11250 1972 AU 08/28-09/02 245 16.5,0.1,10.0 342 0 2.812 0.001 0.15 0.03 EUN 19516 1998 QF80 07/29 61 19.4,20.1 341 15 5.552 0.035 0.32 0.04 MB-I 23587 Abukumado 09/09-09/26 407 8.1,3.1 358 0 3.054 0.001 0.13 0.02 FLOR

Table I. Observing circumstances and results. Pts is the number of data points used in the analysis. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are the average phase angle bisector longitude and latitude. Grp is the asteroid family/group (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 58 years. We observed this asteroid from 2016 August 3 to September 23. The collaborative observations resulted in nine sessions. The bimodal lightcurve has a synodic period of 30.962 ± 0.002 h and amplitude of 0.24 ± 0.03 mag.

23587 Abukumado is a main-belt asteroid discovered on 1995 October 2 by T. Seki. Its orbit has a semi-major axis of about 2.31 AU, eccentricity 0.219, and period of about 3.52 years. We

observed this asteroid from 2016 September 9-26. The (11250) 1972 AU is a main-belt asteroid discovered on 1972 collaborative observations resulted in eight sessions. Our result is January 14 by L. Kohoutek. Its orbit has a semi-major axis of a bimodal lightcurve phased to 3.054 ± 0.001 h and amplitude of about 2.59 AU, eccentricity 0.172, and period of about 4.18 years. 0.13 ± 0.04 mag. We observed this asteroid from 2016 August 28 to September 2. The collaborative observations resulted in four sessions. The result is a bimodal lightcurve with a synodic period 2.812 ± 0.001 h and amplitude of 0.15 ± 0.03 mag.

References

JPL (2016). Small-Body Database Browser. http://ssd.jpl.nasa.gov/sbdb.cgi#top (19516) 1998 QF80 is a main-belt asteroid discovered on 1998 Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid August 24 by LINEAR. Its orbit has a semi-major axis of about Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sept. 2.345 AU, eccentricity 0.266, and period of about 3.59 years. We http://www.minorplanet.info/lightcurvedatabase.html observed this asteroid on 2016 July 29. The collaborative observations resulted in a single session. The result of our analysis Warner, B.D. (2013). MPO Software, MPO Canopus version is a bimodal lightcurve with a synodic period of 5.551 ± 0.034 h 10.4.4.0 Bdw Publishing. http://minorplanetobserver.com and amplitude of 0.32 ± 0.04 mag.

Minor Planet Bulletin 44 (2017) 59 3637 O’MEARA: NEW BINARY CANDIDATE

Amadeo Aznar Macías APT Observatory Group, SPAIN [email protected]

(Received: 2016 October 13 Revised: 2016 November 22)

CCD photometric observations made in 2016 August and September of 3637 O’Meara give some indications that this object could be a binary asteroid. Under the hypothesis that the binary interpretation is correct and not due to a systematic effect, the data suggest the primary lightcurve could have a period of 4.118 ± 0.001 h and an amplitude of 0.25 ± 0.09 magnitudes. The orbital period of the satellite could be 13.8252 ± 0.0021 hours. Based on mutual events ranging from 0.28 to 0.33 mag, the estimated effective diameter ratio of the two bodies is Ds/Dp ≥ 0.59 ± 0.07.

Minor planet 3637 O´Meara is a member of the Eumonia orbital group. It was observed as part of the main-belt asteroid (MBA) lightcurve campaign of APT-Observatory Group, which concentrates efforts on analysis of main-belt asteroids as well as near-Earth objects. There is one entry in the asteroid lightcurve database (LCDB; Warner et al., 2009) for O’Meara, which is from Behrend (2008). He reported a period of 5.49 h. This result is based on an incomplete lightcurve that shows the typical bimodal shape and amplitude of 0.25 mag.

Observations were made using a 0.25-m Schmidt-Cassegrain telescope with SBIG ST9XE and adaptive optics. The 200-second exposures were guided and made without a filter. All images were flat-fielded with bias and dark images subtracted. Photometric reduction was done using MPO Canopus. Linking of the sessions was aided by the Comp Star Selector utility using near solar-color comparison stars (five in each session). The MPOSC3 star catalog The dual-period analysis found a primary solution of P1 = 4.118 ± was used for comparison star magnitudes (see Warner, 2007). 0.025 hours and amplitude of A1 = 0.25 ± 0.09 mag. Assuming an equatorial view, the a/b axis size ratio is 1.257 (Zappala et al., The “StarBGone” routine within MPO Canopus was used to 1990). The presumed orbital period is PORB = 13.8252 ± 0.0021 h subtract stars that merged with the asteroid. MPO Canopus was with AORB = 0.28-0.33 magnitudes. The secondary lightcurve also used for period analysis. This software employs a FALC shows two attenuations that might indicate mutual events due to a Fourier analysis algorithm developed by Harris (Harris et al., satellite. 1989). The initial two sessions did not show any sign of binary nature. These observations were made at the end of August. However, in the third session there was an apparent deviation from the main lightcurve. After accumulating several sessions, it was very difficult to get a satisfactory composite lightcurve using a single period.

Difficulties with imperfect star subtraction can sometimes mimic transit events, thus the suggestion of the binary nature for this object must be considered with a critical eye. Under the assumption that the asteroid is a binary, the dual-period search in MPO Canopus was used to find the rotation period of a primary and orbital period of a satellite. An iterative process was used in which, after obtaining an initial rotation period for the primary (the dominant period), the resulting Fourier model was subtracted from the data set in order to get a second period. The second period was then subtracted from data set in order to improve the dominant period. This process continued until both periods converge to a final value.

Table I shows the observation circumstances and results for the suspected primary of the binary system.

Minor Planet Bulletin 44 (2017) 60

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 3637 O’Meara 08/22-09/13 445 20.3,24.2 294 18 4.118 0.025 0.25 0.09

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). The period is for the presumed primary of a binary system.

Acknowledgements

I would like to express my gratitude to Brian Warner for supporting LCDB as main database for study of asteroids.

References

Behrend, R. (2008). Observatoire de Geneve web site. http://obswww.unige.ch/~behrend/page_cou.html

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Using the shallower event and: Warner, B.D. (2007). “Initial Results of a Dedicated H-G Program.” Minor Planet Bul. 34, 113-119. 0.4Δm Ds Dp ≥ 10 − 1 Zappala, V., Cellini, A., Barucci, A.M., Fulchignoni, M., Lupishko, D.E. (1990). “An analysis of the amplitude-phase gives an approximate diameter ratio (Ds/Dp) of 0.55 ± 0.09. relationship among asteroids.” Astron. Astrophys. 231, 548-560. New observations€ of this object at future apparitions will be needed in order to improve the analysis and confirm its binary nature.

LIGHTCURVE ANALYSIS FROM APT OBSERVATORY The APT Observatory Group is made up of two observatories. The GROUP FOR NINE MAINBELT ASTEROIDS: Isaac Aznar Observatory is located in Centro Astronómico del 2016 JULY-SEPTEMBER. Alto Turia, Aras de los Olmos, Valencia, Spain. It is 1270 meters ROTATION PERIOD AND PHYSICAL PARAMETERS. above sea level under a very dark and high quality night sky (~21.7 magnitudes/arcsec2). The observatory is equipped with a Amadeo Aznar Macías 0.35-m telescope, STL-1001E CCD camera, and adaptive optics APT Observatory Group, SPAIN system. Pixel resolution is 1.44 arcseconds. The POP-Punto de [email protected] Observación de Puçol, Puçol, Spain, is an urban observatory equipped with a 0.25-m telescope, SBIG ST-9 CCD camera, and (Received: 2016 October 13) adaptive optics system. Pixel resolution is 1.56 arcseconds. Table I summarizes the telescope/CCD camera combinations. Lightcurves of nine main-belt asteroids (MBAs) obtained at APT-Observatory Group from 2016 July- Observatory Telescope (m) CCD + Accessories September were analyzed for rotation period, amplitude, and axis ratios. OIA Obs. Isaac Aznar 0.35m SCT SBIG STL1001E+AO POP Punto Obs. Puçol 0.25m SCT SBIG ST9XE+AO Table I. Equipment used for asteroid photometry. CCD photometric observations of nine main-belt asteroids (MBAs) were made by APT Observatory Group 2016 July to All images were obtained in 1x1 binning mode and were taken September. Asteroids were selected based on the U (quality) code without any photometric filter. Dark, bias, and twilight sky flat- given in the asteroid lightcurve database (LCDB; Warner et al., field frames were applied to each raw image. The resulting SNR 2009). Most objects had ratings of U = 2 or 3. However, some values allowed obtaining lightcurves with low data dispersion. asteroids were not in the LCDB or had no U rating. Despite being rated U = 3, it can be worthwhile to observe an asteroid since the Data reduction was done using MPO Canopus, which implements shape and/or amplitude of the lightcurve often changes from one the FALC algorithm developed by Harris (Harris et al., 1989). The apparition to another. These changes are important when modeling Comp Star Selector utility in MPO Canopus found up to five an asteroid for its actual shape. comparison stars of near solar-color for differential photometry. Comparison star magnitudes were taken from the APASS catalog (Henden et al., 2009) or MPOSC3 (Warner, 2007) depending on Minor Planet Bulletin 44 (2017) 61

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. D a/b b/c 565 Marbachia 07/17-07/28 740 10.7,14.3 275 11 4.588 0.001 0.70 0.09 27.3 1.63 0.62 1293 Sonja 07/09-07/10 99 18.5,18.0 308 8 2.881 0.02 0.19 0.01 7.9* 1.12 1.02 1346 Gotha 09/06-09/18 158 13.6,17.3 314 7 2.642 0.001 0.16 0.04 14.2 1.13 1.03 2189 Zaragoza 07/02-07/06 285 14.1,12.1 301 5 4.927 0.0006 0.86 0.03 6.0 1.75 0.54 3042 Zelinsky 08/08 37 6.6 313 8 4.468 0.094 0.14 0.01 5.7 1.12 1.02 3232 Brest 09/28-10/02 181 5.2,7.3 352 4 5.288 0.004 0.25 0.04 16.6* 1.24 1.04 4923 Clarke 07/30-08/01 62 17.4,18.3 288 10 3.143 0.016 0.14 0.04 3.0 1.09 1.01 10306 Pagnol 07/16-08/01 163 5.9,5.6,7.7 298 11 4.79 0.01 0.27 0.05 9.1* 1.23 1.04 19516 1998 QF80 07/26-07/30 375 21.4,19.7 330 8 5.438 0.001 0.33 0.02 16.2 1.26 1.06

Table II. Observing circumstances and results. Pts is the number of data points used in the analysis. The phase angle values are for the first and last date, unless a minimum (second value) was reached. LPAB and BPAB are the average phase angle bisector longitude and latitude. Period is in hours. Amp is peak-to-peak amplitude in magnitudes. D is the estimated diameter (km). * indicates diameter is from the JPL

Small Bodies Node. The other diameters were calculated from the reported H and pV values. The last two columns give the a/b and b/c ratios for an assumed triaxial ellipsoid viewed equatorially based on the amplitude. availability of comparison stars. The nightly zero points for both catalogs have been found to be generally consistent to about ± 0.05 mag or better, but on occasion reach 0.1 mag and more.

The StarBGone star subtraction feature in MPO Canopus was used to remove or reduce the effect of stars located in the asteroid path. This technique is most effective when the star’s SNR is equal to or less than asteroid SNR. (Aznar, 2013).

Table II gives the observing circumstances and results for each asteroid. See Aznar (2016) for details concerning the derivation of the asteroid axis ratios as determined by the lightcurve amplitude.

565 Marbachia. The period for Marbachia has been reported on many occasions, all of them being about 4.5 hours. Hanus et al., (2016) found a sidereal rotation period of 4.587 h. The synodic period found from our analysis using ten sessions is in agreement with those earlier results. 1346 Gotha. Binzel (1987) was the first to report a period for Gotha (11.19 h). Waszczak et al. (2015) found a period of 2.6405 h. Our result matches the more recent result. Given the low amplitude of 0.16 mag, this asteroid has an almost spherical form, assuming it was viewed equatorially.

1293 Sonja. Five previously reported periods for this asteroid were all approximately 2.87 h (Warner et al., 2009). Our result is very similar. The lightcurve shows a bimodal shape with a maximum amplitude of 0.19 mag at a phase angle of 18º. As noted by Zappala et al. (1990), the amplitude at 0° phase angle would be smaller. (2189) Zaragoza. Previous reports for the period of this asteroid include Higgins (2011; 4.934 h) and Pravec et al. (2016; 4.9282 h). Our period is consistent with those earlier results.

Minor Planet Bulletin 44 (2017) 62

(4923) Clarke. Pravec et al. (2013) found a period of 3.1787 h while Waszczak et al. (2015) reported a period of 27.2531 h. Our analysis found a rotation period of 3.143 ± 0.016 h, which is in close agreement with Pravec et al. Assuming an equatorial viewing aspect, the low amplitude of 0.14 mag indicates a nearly spheroidal shape for the asteroid.

(3042) Zelinsky. Pravec et al. (2016) found a period of 5.3248 h for this asteroid. The analysis of our data found 4.468 hours. However, we obtained a small data set due to bad weather and our result also includes a large gap in the lightcurve coverage.

(10306) Pagnol. There were no entries in the LCDB for this asteroid. We derived a rotation period of 4.79 ± 0.01 h with an amplitude of 0.27 mag. The lightcurve shows a typical bimodal shape; its amplitude suggests a semi-elongated shape.

3232 Brest. There were no previous entries in the LCDB (Warner et al., 2009). Our lightcurve, composed by 181 points, shows a mostly flat shape with an amplitude of 0.25 mag and period of 5.288 ± 0.004 h. Although our solution could be right, we suggest observations at future apparitions to confirm this result.

(19516) 1998 QF80. Pravec et al. (2016) found a period of about 5.438 h for this asteroid. Analysis of our data found a period of 5.438 ± 0.001 h. The lightcurve shows a bimodal shape with a maximum amplitude of 0.33 magnitudes.

Minor Planet Bulletin 44 (2017) 63

Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry.” Astron. J. 150, A75.

Zappala, V., Cellini, A., Barucci, A.M., Fulchignoni, M., Lupishko, D.E. (1990). “An analysis of the amplitude-phase relationship among asteroids.” Astron. Astrophys. 231, 548-560.

ROTATION PERIOD DETERMINATION OF ASTEROIDS (8360) 1990 FD1 AND (11386) 1998 TA18

Riccardo Papini Carpione Observatory (K49) via Potente 52, 50026 San Casciano in val di Pesa (FI), ITALY [email protected] Acknowledgements Alessandro Marchini Astronomical Observatory, DSFTA - University of Siena (K54) I would like to express my gratitude to Brian Warner for Via Roma 56, 53100 – Siena, ITALY supporting LCDB as main database for study of asteroids. I would like to express my gratitude to Irina Belscaka (Institute of Fabio Salvaggio Astronomy of Kharkiv National University, Department of 21047 – Saronno, ITALY Physics of Asteroids and Comets) for her support in axis size relationship calculation. (Received: 2016 October 10)

References Photometric observations were made in 2016 April and October of the main-belt asteroids (8360) 1990 FD1 and Aznar. A. (2013). “Lightcurve of 3422 Reid Using Star (11386) 1998 TA18. For 1990 FD1, analysis of the data Subtraction Techniques.” Minor Planet Bull. 40, 214-215. found a period of 8.094 ± 0.003 h; for 1998 TA18 a likely period of 15.943 ± 0.003 h was found. Aznar, A. (2016). “Parameters of Rotation Shapes of Main-belt Asteroids from APT Observatory Group: Second Quarter 2016.” Photometric observations of the main-belt asteroids (8360) 1990 Minor Planet Bull. 43, 350-353. FD1 and (11386) 1998 TA18 were taken at the Astronomical Observatory of the University of Siena (K54), Italy, with a 0.30 m Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.” f/5.6 Maksutov-Cassegrain telescope equipped with a SBIG STL- Icarus 72, 135-208. 6303E NABG CCD camera and clear filter. The pixel scale was 2.26 arcsec in binning 2x2. Exposure time was 300 seconds. Table Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., I gives the observation circumstances and results. Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K.W. (1989). “Photoelectric Observations of Differential photometry measurements were performed using the Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Comp Star Selector (CSS) procedure in MPO Canopus (Warner, 2012) that allows selecting of up to five comparison stars of near Hanus, J., Durech, J., Oszkiewicz, D.A., Behrend, R., Carry, B., solar color. The magnitudes from the CMC-15 catalog were used Delbo, M., Adam, O., Afonina, V., Anquetin, R., Antonini, P., and for the comparison stars. Period analysis was performed using 159 coauthors. (2016). “New and updated convex shape models of MPO Canopus and its FALC (Fourier Analysis for Lightcurves) asteroids based on optical data from a large collaboration algorithm (Harris et al., 1989). Additional adjustments of the network.” Astron. Astrophys. 586, A108. magnitude zero-points for each data set were carried out in order to reach the minimum RMS value from the Fourier analysis and so Higgins, D. (2011). “Period Determination of Asteroid Targets achieve the best alignment among lightcurves. Observed at Hunters Hill Observatory: May 2009 - September 2010.” Minor Planet Bull. 38, 41-46. A search of the Asteroid Lightcurve Database (LCDB; Warner et al., 2009) and literature found no previous entries. Pravec, P., Wolf, M., Sarounova, L. (2013, 2016). http://www.asu.cas.cz/~ppravec/neo.htm (8360) 1990 FD1 was discovered on 1990 March 26 by Atsushi Sugie, a Japanese astronomer, at the Dynic Astronomical Warner, B.D. (2007). “Initial Results of a Dedicated H-G Observatory. It orbits with a semi-major axis of about 2.64 AU, Program.” Minor Planet Bull. 34, 113-119. eccentricity 0.12, and a period of 4.3 years (JPL, 2014). Observations were made on three nights from 2016 April 5-10 Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid with a total of 157 useful data points collected over that time. The lightcurve database.” Icarus 202, 134-146. Updated 2016 Sept. period analysis yielded a few possible solutions with nearly http://www.MinorPlanet.info/lightcurvedatabase.html comparable RMS values. We concluded that the most likely value of the synodic period for (8360) 1990 FD1 is associated with a Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., bimodal lightcurve phased to 8.094 ± 0.003 h with an amplitude of Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., 0.26 ± 0.03 mag. Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light

Minor Planet Bulletin 44 (2017) 64

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 8360 1990 FD1 04/05-04/10 157 11.7,10.6 209 19 8.094 0.003 0.26 0.03 11386 1998 TA18 09/29-10/04 231 10.0,8.9 12 11 15.943 0.003 0.61 0.01

Table II. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude.

The period analysis yielded several possible solutions with comparable RMS errors. We concluded that the most likely value of the synodic period is associated with a bimodal lightcurve phased to 15.943 ± 0.003 h with an amplitude of 0.61 ± 0.01 mag.

Acknowledgments

The authors want to thank here Teodora Palmas, a student of the course in Physics and Advanced Technologies, who looked after the collection and analysis of data during her internship activities at the Astronomical Observatory of the University of Siena.

References

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K. (1989). “Photoelectric observations of asteroids 3, (11386) 1998 TA18 is a main-belt asteroid discovered on 1998 24, 60, 261, and 863.” Icarus 77, 171-186. October 12 by S. Ueda and H. Kaneda, two Japanese astronomers, at Kushiro. It orbits with a semi-major axis of about 2.35 AU, JPL (2014). Small-Body Database Browser. eccentricity 0.28, and a period of 3.6 years (JPL, 2014). http://ssd.jpl.nasa.gov/sbdb.cgi#top Observations were made on four nights from 2016 September 29 thru October 4 with a total of 231 data points collected. Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid lightcurve database.” Icarus 202, 134-146. Updated 2016 Sept. http://www.minorplanet.info/lightcurvedatabase.html

Warner, B.D. (2012). MPO Software, Canopus version 10.4.1.9. Bdw Publishing. http://minorplanetobserver.com

Minor Planet Bulletin 44 (2017) 65

LIGHTCURVE ANALYSIS FOR objects of such size have very short rotation periods. NEAR-EARTH ASTEROID 2015 SZ2

Volodymyr Reshetnyk, Vira Godunova, Maxim Andreev ICAMER Observatory of NASU (MPC B18) 27 Acad Zabolotnoho Str. Kyiv, 03680 UKRAINE [email protected]

Vitalii Polyakov Research and Training Center for Applied Informatics of NASU Kyiv, UKRAINE

(Received: 15 October 2016)

We present analysis of photometric observations obtained in 2015 September at the Terskol Observatory of the fast rotating asteroid 2015 SZ2. We found the rotation period for the NEA to be P = 0.03832 ± 0.00002 h with an lightcurve amplitude of 0.32 ± 0.02 mag. We also found a color index of V-R = 0.37 ± 0.02.

Asteroid 2015 SZ2 was first observed by Catalina Sky Survey on 2015 September 23. This is a small Apollo-type asteroid with an absolute magnitude (H) of 25.4, which suggests – depending on albedo – a diameter of 25-56 meters. It passed close by the Earth (within 0.0034 au) on 2015 September 30. Taking into account that this asteroid is on NASA's list of potential human mission targets (NHATS), studies of its physical properties are very important. The Asteroid Lightcurve Database (LCDB; Warner et al., 2009) did not contain any previously reported results for 2015 SZ2, so our findings appear to be the first reported information on this near-Earth object. Acknowledgements

Follow-up photometry of 2015 SZ2 was carried out at the Terskol This work has been supported by the NASU-KNU project No. Observatory over one night on 2015 September 28 (18:36-21:24 0114U003875. V. Godunova acknowledges a grant from the UT). Observations were obtained using the 60-cm Cassegrain European Astronomical Society awarded to her in 2015. telescope (Zeiss-600) and a SBIG STL-1001 CCD with 1024x1024 24-micron pixels. This gave a field of view of References 10.9x10.9 arcmin. During the observations the phase angle ranged from 19.3 to 20.4 degrees. The asteroid’s V magnitude was about Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). 15.3. V, R, and clear filters were used for the 5-10 s exposures. “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258. Data processing was performed using MaxIm DL and our own software. A total of 620 data points were employed in the analysis. Hergenrother, C.W., Whiteley, R.J. (2011). “A survey of small Images were calibrated with bias, flat, and dark frames. Three fast rotating asteroids among the near-Earth asteroid population.” photometric standard stars from the NOMAD catalog were used to Icarus 214, 194-209. reduce data to R band. Observations with Johnson-Cousins V and JPL-NASA (2016). NHATS list R filters allowed us to calculate a mean value of a color index http://neo.jpl.nasa.gov/nhats/ V- R = 0.37 ± 0.02. Lomb, N.R. (1976). “Least-squares frequency analysis of To find the periodicity in the lightcurve, the PDM technique was unequally spaced data.” Ap&SS 39, 447-462. applied (Stellingwerf, 1978). Furthermore, we checked the result with the Lomb normalized periodogram method (Lomb, 1976) and Stellingwerf, R.F. (1978). “Period determination using phase Ө-statistic. It was found that all these techniques produced a dispersion minimization.” ApJ 224, 953-960. similar result: a synodic rotation period of 0.03832 ± 0.00002 h and amplitude of 0.32 ± 0.02 mag. The estimated diameter of 2015 Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid SZ2 ranges from 25 to 56 meters, so a super-fast rotation period is lightcurve database.” Icarus 202, 134-146. Updated 2016 Sept 6. not unusual. Hergenrother and Whiteley (2011) found that many http://www.minorplanet.info/lightcurvedatabase.html

Number Name 2015 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. V-R Err 2015 SZ2 09/28 620 19.3,20.4 228 33 0.03832 0.0002 0.32 0.02 0.37 0.02

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle values are for the start and end of the single night of observations. LPAB and BPAB are the average phase angle bisector longitude and latitude (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 66

ROTATION PERIOD DETERMINATION arcsec in binning 2x2. Exposures were 300 seconds. A total of 490 FOR 4963 KANROKU data points were collected.

Alessandro Marchini, Teodora Palmas Images were calibrated with bias, flat, and dark frames. Data Astronomical Observatory, DSFTA - University of Siena (K54) processing, including reduction to R band, and period analysis was Via Roma 56, 53100 - Siena, ITALY performed using MPO Canopus (BDW Publishing, 2012). [email protected] Differential photometry measurements were performed using the Comp Star Selector (CSS) procedure in MPO Canopus that allows Lorenzo Franco selecting of up to five comparison stars of near solar color. Balzaretto Observatory (A81), Rome, ITALY Additional adjustments of the magnitude zero-points for each night were made to find the minimum RMS value from the Riccardo Papini Fourier analysis. Carpione Observatory (K49) Spedaletto, Florence, ITALY

Fabio Salvaggio 21047 - Saronno, ITALY

(Received: 2016 October 14)

Photometric observations of the main-belt asteroid 4963 Kanroku from Italy in 2016 August revealed a trimodal lightcurve phased to 2.616 ± 0.001 hours as the most likely solution for the synodic rotation period of the asteroid. From photometric sparse data we also derived H = 12.00 ± 0.03 and G = 0.28 ± 0.03.

The main-belt asteroid 4963 Kanroku (1977 DR1) was discovered at Kiso on 1977 February 18 by H. Kosai and K. Hurukawa. It is named for a Pekche priest who presented books on calendar- making, astronomy, geography, and divination to the Japanese Government in 602, and taught the Japanese the algorithm of the luni-solar calendar used in China (MPC 22504). The asteroid orbits with a semi-major axis of about 2.600 AU, eccentricity 0.164, and a period of 4.19 years.

Its absolute magnitude is H = 11.9 (JPL, 2016; MPC, 2016) while the WISE satellite infrared radiometry reports a value of H = 12.40 with a diameter of 11.306 ± 0.034 km based on an optical albedo of 0.152 ± 0.014 (Masiero et al., 2011).

The period analysis strongly favored a solution near 2.6 hours, so we concluded that the most likely synodic period is associated with a trimodal lightcurve phased to 2.616 ± 0.001 hours and amplitude of 0.13 ± 0.01 mag. A search of the asteroid lightcurve database (LCDB; Warner et al., 2009) indicates that our results may be the first reported lightcurve observations and results for this object.

During period analysis, we found some small attenuation events in the lightcurves that cannot be confirmed with the existing data. Observations at future oppositions will be required to verify the possibility of the asteroid being binary. Using sparse photometric data from the Catalina Sky Survey (MPC 703; CSS, 2016) we derived H = 12.00 ± 0.03 and G = 0.28 Acknowledgments ± 0.03; the H value is close to that one from JPL Small-Body Database Browser. The authors want to thank Teodora Palmas, a student of the course in Physics and Advanced Technologies, for her efforts in the Observations at the Astronomical Observatory of the University of analysis of data and the writing of this article during her internship Siena were carried out on seven nights from 2016 August 13-27 activities at the Astronomical Observatory of the University of using a 0.30-m f/5.6 Maksutov-Cassegrain telescope, SBIG STL- Siena. 6303E CCD camera, and clear filter; the pixel scale was 2.32 Minor Planet Bulletin 44 (2017) 67

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. 4963 Kanroku 08/13-08/27 490 7.2,0.5 334 0 2.616 0.001 0.13 0.01

Table I. Observing circumstances and results. Pts is the number of data points used in the analysis. The phase angle (α) is given at the start

and end of each date range. LPAB and BPAB are the average phase angle bisector longitude and latitude.

References “Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters.” Astrophys. J. 741, A68. Catalina Sky Survey (2016). http://www.lpl.arizona.edu/css/ MPC (2016). MPC Database. http://www.minorplanetcenter.net/db_search/ JPL (2016). Small-Body Database Browser. http://ssd.jpl.nasa.gov/sbdb.cgi#top Warner, B.D. (2012). MPO Software, MPO Canopus v10.4.1.9. Bdw Publishing. http://minorplanetobserver.com Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., Dailey, J., Eisenhardt, P.R.M., McMillan, R.S., Spahr, T.B., Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid Skrutskie, M.F., Tholen, D., Walker, R.G., Wright, E.L., DeBaun, lightcurve database.” Icarus 202, 134-146. Updated 2016 Sept. E., Elsbury, D., Gautier, T., IV, Gomillion, S., Wilkins, A. (2011). http://www.minorplanet.info/lightcurvedatabase.html

LIGHTCURVES AND ROTATION PERIODS (APASS; Henden et al., 2009), Data Release 9 were used. In some FOR SIX ASTEROIDS instances, small zero point adjustments were necessary in order to achieve the best match between individual data sets in terms of Vladimir Benishek minimum RMS residual of a Fourier fit. Belgrade Astronomical Observatory Volgina 7, 11060 Belgrade 38, SERBIA Table I gives the observing circumstances and results. [email protected] 3976 Lise. No previous records on rotation period determinations (Received: 2016 October 15) were found for this main-belt asteroid discovered in 1983. A total of 14 photometric data sets was obtained from 2016 August 27 CCD photometric observations of six asteroids were until September 28, which provided a good fit to an asymmetrical conducted from 2016 June until 2016 October. A review lightcurve phased to a period of P = 15.6912 ± 0.0007 h and with of the results of data analysis is presented. an amplitude of 0.23 mag.

Photometric observations of six asteroids were conducted at Sopot 4524 Barklajdetolli. The previous observations conducted by Pray Astronomical Observatory (SAO) in the interval between 2016 and Durkee over 16 nights from 2009 June through September and June and October, in order to determine their synodic rotation corresponding period analysis (Pray and Durkee, 2010) show this periods. For this purpose, a 0.35-m Meade LX200GPS Schmidt- main-belt asteroid to be a slow rotator with a synodic period of Cassegrain telescope with an f/6.3 focal reducer and a SBIG ST-8 1069 ± 3 h, which classifies it as one of the slowest rotating XME CCD camera were employed. The exposures were unfiltered asteroids ever measured. As the predicted magnitude of this and unguided for all photometric targets. The camera was operated asteroid should have been of V ~ 15.0 at its brightest during 2016 in a 2x2 binning mode providing an image scale of 1.66 apparition, the author has assessed that this could be a good arcsec/pixel. Prior to measurements, all images were corrected opportunity to improve, if possible, the previously found period by using dark and flat field frames. providing denser photometric observations than it was the case before. Photometric reduction, lightcurve construction, and period analysis were conducted using MPO Canopus (Warner, 2015). The observations started on 2016 June 18 and concluded on Differential photometry with up to five comparison stars of near September 30, i.e. from the phase angle 13.7 deg. before the solar color (0.5 ≤ B-V ≤ 0.9) was performed using the Comparison opposition, up to a quite high post-opposition phase angle of 29.1 Star Selector (CSS) utility. This helped ensure a satisfactory deg. Since it was known that the rotation of the target is quality level of night-to-night zero point calibrations and undoubtedly very slow, the observation strategy was to take only a correlation of the measurements within the standard magnitude few data points per night in order to save observing time. This framework. To calibrate field comparison stars, the Johnson V resulted in a total of 45 individual data sets. Since the total range magnitudes from the AAVSO Photometric All-Sky Survey catalog of the covered phase angles is rather large it is quite reasonable to

Number Name 2016 mm/dd Phase LPAB BPAB Period (h) P.E. Amp A.E. Grp 3976 Lise 08/27-09/29 7.5,13.8 337 14 15.6912 0.0007 0.23 0.02 MB-O 4524 Barklajdetolli 06/18-09/30 13.7,6.4,29.1 293 7 970 3 1.05 0.05 FLOR 5349 Paulharris 09/12-09/15 29.5,29.2 34 13 7.890 0.005 0.18 0.02 M-C 15350 Naganuma 10/06 15.8 33 -1 2.587 0.008 0.17 0.02 MB-I 23721 1998 HQ27 07/30-08/05 16.8,13.8 328 8 5.3034 0.0009 0.17 0.02 FLOR 2016 LX48 09/29-10/06 38.6,31.6 19 19 5.6799 0.0008 0.47 0.03 NEA

Table I. Observing circumstances and results. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. If a single value is given, the phase angle did not change significantly and the average

value is given. LPAB and BPAB are the average phase angle bisector longitude and latitude. Grp is the asteroid family/group (Warner et al., 2009). Minor Planet Bulletin 44 (2017) 68 expect that the amplitude and shape of the lightcurve have been Warner, B.D., Harris, A.W., Pravec, P. (2009). Icarus 202, 134- somewhat altered within the corresponding time frame. For this 146. Updated 2016 September 6. reason, the resulting lightcurve represents an averaged result over http://www.MinorPlanet.info/lightcurvedatabase.html the specified period of time. Since the amplitude of the obtained lightcurve has a fairly large value of 1.05 mag., as it was also Warner, B.D. (2015). MPO Canopus software version. ascertained by Pray and Durkee from the 2009 apparition data 10.4.7.6.http://www.bdwpublishing.com (1.26 mag.) there is no doubt that the bimodal solution has the advantage over the monomodal one of 483 ± 1 h that also stands out in the period spectrum (Harris et al., 2014). The corresponding period of the resulting bimodal lightcurve is found to be 970 ± 3 h, which is a shorter period than that found from 2009 observations.

5349 Paulharris. No exact result for period of this Mars-crosser was obtained previously. In order to find the period the photometric observations were conducted over three nights in 2016 September providing a good fit to a bimodal lightcurve phased to 7.890 ± 0.005 hours and with an amplitude of 0.18 mag.

15350 Naganuma. This target was observed at the SAO over a single night in October 2016 within the framework of the Photometric Survey for Asynchronous Binary Asteroids (BinAstPhot Survey). No significant deviations that may indicate a binary nature of this target were detected. The bimodal solution found for period (2.587 ± 0.008 h) is in good accordance with the values found from the observations carried out in some previous apparitions: 2.5835 h (Pray et al., 2006) and 2.58348 h (Pravec, 2010).

(23721) 1998 HQ27. Another target observed within the BinAstPhot Survey. It was observed at the SAO over 5 nights in late July and early August 2016. Period analysis of the collected data yielded a bimodal lightcurve phased to a period of 5.3034 ± 0.0009 h with an amplitude of 0.17 mag. The period result derived by Pravec using the SAO data is 5.3036 ± 0.0007 h (Pravec, 2016).

2016 LX48. This recently discovered potentially hazardous asteroid (PHA) was observed over 6 nights in 2016 late September and early October, which led to an unambiguous bimodal solution for period of 5.6799 ± 0.0008 h. The corresponding lightcurve has an amplitude of 0.47 mag.

References

Harris, A.W., Pravec, P., Galád, A., Skiff, B.A., Warner, B.D., Világi, J., Gajdoš, Š., Carbognani, A., Hornoch, K., Kušnirák, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics of an asteroid lightcurve.” Icarus 235, 55-59.

Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). “The AAVSO Photometric All-Sky Survey (APASS).” https://www.aavso.org/apass

Pravec, P. (2010, 2016). Photometric Survey for Asynchronous Binary Asteroids web site. http://www.asu.cas.cz/~ppravec/newres.txt

Pray, D.P., Galad, A., Gajdos, S., Vilagi, J., Cooney, W., Gross, J., Terrel, D., Higgins, D., Husarik, M., Kusnirak, P. (2006). “Lightcurve analysis of asteroids 53, 698, 1016, 1523, 1950, 4608, 5080 6170, 7760, 8213, 11271, 14257, 15350 and 17509.” Minor Planet Bul. 33, 92-95.

Pray, D.P., Durkee, R.I. (2010). “The Extremely Long Period of 4524 Barklajdetolli.” Minor Planet Bul. 37, 35.

Minor Planet Bulletin 44 (2017) 69

ASTEROID PHOTOMETRY RESULTS Our observations were obtained with the three Celestron 0.35-m FROM ETSCORN OBSEVATORY telescopes and SBIG CCD cameras at Etscorn Campus Observatory (Klinglesmith and Franco, 2016). The images were Daniel A. Klinglesmith III processed and calibrated using MPO Canopus 10.4.7.6 (Warner, Etscorn Campus Observatory 2015). The exposures were between 180 and 420 seconds through New Mexico Tech clear filters depending on the brightness of the asteroids. The 101 East Road multi-night data sets for each asteroid were combined with the Socorro, NM 87801 USA FALC algorithm (Harris et al., 1989) within MPO Canopus to [email protected] provide synodic periods for each asteroid.

(Received: 15 October 2016) Discovery information was obtained from the JPL small bodies node (JPL, 2016). Observations of these seven asteroids were We obtained lightcurves for seven asteroids observed obtained because that was suggested as Spin/Shape. Table I gives between 2016 July and October. Synodic rotation the observing circumstances and results for each asteroid obtained periods and lightcurve amplitudes are reported for 775 for this paper. Table II again gives our results along with those Lumiere, 1044 Teutonia, 1084 Tamariwa, 1095 Tulipa, obtained in previous efforts at Estcorn Observatory or by other 1293 Sonja, 3105 Stumpff, and 4132 Bartok. authors.

We made CCD photometric observations of seven asteroids that were selected from the lists of shape/spin modeling (SSMO) opportunities given by Warner et al. (2016a, 2016b) in the Minor Planet Bulletin. Asteroids with known periods of less than 8 hours were selected based on brightness and modeling opportunities. This allowed the possibility of at least one cycle to be obtained per night, provided we could observe the object the entire night.

Minor Planet Bulletin 44 (2017) 70

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. 775 Lumiere 09/18-09/19 140 6.8,7.1 339 8 6.075 0.004 0.25 0.01 1044 Teutonia 10/11-10/12 224 3.3,3.7 13 -4 3.158 0.001 0.25 0.01 1084 Tamariwa 09/10-09/28 392 2.1,0.7,6.6 352 1 6.195 0.001 0.28 0.01 1095 Tulipa 07/12-07/23 116 11.4,14.0 262 12 2.787 0.001 0.19 0.02 1293 Sonja 09/06-09/09 135 21.1,22.5 321 9 2.876 0.001 0.21 0.01 3105 Stumpff 10/01-10/08 331 12.6,16.7 352 -6 5.036 0.001 0.46 0.03 4132 Bartok 09/05-09/09 142 8.8,10.3 331 11 3.297 0.001 0.37 0.03

775 Lumiere is a main-belt asteroid discovered by J. Lagrula at 1084 Tamariwa is a main-belt asteroid discovered by S. Nice on 1914 Jan 6. It is also known as 1914 TX. We observed Belyavskij at Simeis on 1926 Feb 12. It is also known as 1926 CC. 775 Lumiere on two nights: 2016 Sep 18 and 19. We obtained a We observed 10844 Tamariwa on five nights between 2016 Sep synodic period of 6.075 ± 0.004 h. and an amplitude of 0.25 mag. 10 and 28. We obtained a synodic period of 6.195 ± 0.001 h and an amplitude of 0.28 mag.

1044 Teutonia is a main-belt asteroid discovered by K. Reinmuth at Heidelberg on 1924 May 10. It is also known as 1924 RO, 1925 1095 Tulipa is a main-belt asteroid discovered by K. Reinmuth at XF, 1929 RP, 1949 KX, 1954 UY1, 1958 RG, 1958 UP, A907 EE. Heidelberg on 1926 Apr 14. It is also known as 1926 GS. We We observed 1044 Teutonia on two nights: 2016 Oct 11 and 12. observed 1095 Tulipa on five nights between 2016 Jul 12 and 23. We obtained a synodic period of 3.158 ± 0.001 h and an amplitude We obtained a synodic period of 2.787 ± 0.001 h and an amplitude of 0.31 mag. of 0.19 mag.

Minor Planet Bulletin 44 (2017) 71

Num Reference Date LPAB BPAB Ph Period Amp 3105 Stumpff is a main-belt asteroid discovered by A. Kopff at 775 This paper 2016 09/18 339 8 7.0 6.075 0.25 Heidelberg on 1907 Aug 8. It is also known as A907 PB. We Binzel 1987 1983 05/14 217 -11 7.4 6.96 0.25 observed 3105 Stumpff on seven nights between 2016 Oct 1 and Behrend 2001 1983 09/13 34 11 15.7 6.1035 0.28 8. We obtained a synodic period of 5.036 ± 0.001 h and an Behrend 2003 2003 03/24 136 -5 16.9 6.1 0.28 amplitude of 0.46 mag. Behrend 2005 2005 07/07 299 0 5.2 6.1 0.2 Behrend 2006 2006 10/21 16 11 5.2 6.103 0.19 1044 This paper 2016 10/11 13 -4 3.5 3.158 0.25 Behrend 2006 2006 01/11 139 5 11.1 3.153 0.27 Betzler 2008 2007 06/08 256 -27 1.0 2.84 0.2 Behrend 2012 2012 11/13 29 -2 9.9 3.18 0.28 Klinglesmith 2014 02/03 116 5 8.9 3.157 0.28 2014 Waszczak 2015 2013 12/27 117 4 8.7 3.1397 0.32 1084 This paper 2016 09/20 352 1 0.7 6.195 0.28 Binzel 1987b 1984 04/28 165 1 9.7 7.08 0.27 Ivarsen 2004 2003 10/15 20 -1 0.8 6.19 0.25 Behrend 2007 2007 10/20 333 2 2.0 6.1961 0.42 Sada 2008a 2007 08/22 327 3 2.0 6.1949 0.3 Stecher 2008 2007 08/03 326 4 8.8 6.22 0.35 Sada 2016 2015 05/06 210 2 7.0 6.195 0.3 1095 This paper 2016 07/15 262 12 12.7 2.787 0.19 Binzel 1987a 1983 02/10 137 -8 3.6 2.77 0.21 Behrend 2005 2005 05/15 220 9 6.7 2.78721 0.21 Benishek 2008 2006 07/20 306 19 5.3 2.7879 0.17 Benishek 2015 2013 12/18 86 -12 4.8 2.7873 0.23 Waszczak 2015 2012 08/28 4.5 0 10.8 2.7872 0.14 4132 Bartok is a main-belt asteroid discovered by J. Alu at 1293 This paper 2016 09/08 321 9 21.8 2.876 0.21 Palomar Observatory. It is also known as 1988 EH. We observed Higgens 2007 2006 06/24 298 7 20.5 2.878 0.21 4132 Bartok on three nights between 2016 Sep 5 and 9. We Behrend 2006 2006 08/01 305 9 8.3 2.8785 0.14 obtained a synodic period of 3.297 ± 0.001 h with an amplitude of Benishek 2008 2006 08/20 309 9 17.2 2.879 0.15 0.37 mag. Pravec 2008 2008 02/02 137 -7 3.5 2.87797 0.16 Pravec 2016 2016 07/09 308 80 18.5 2.8758 0.18 3105 This paper 2016 10/05 352 -6 14.6 5.036 0.46 Oey 2007 2006 11/14 42 -9 8.3 5.0369 0.35 Pravec 2012 2012 04/21 224 9 7.9 5.044 0.37 Pravec 2015 2016 03/15 180 6 3.8 5.037 0.32 4132 This paper 2016 09/06 331 11 9.7 3.297 0.37 Skiff 2011 2011 04/25 224 22 9.3 3.297 0.32 Warner 2014 2014 04/14 158 -2 21.0 3.297 0.41 Behrend 2014 2014 03/02 155 -10 6.4 3.2965 0.35 Table II. Previous results for the SSMO asteroids observed for this paper. The date is the approximate mid-date of the observing run as reported in the respective papers. Ph is solar phase angle. 1293 Sonja is a main-belt asteroid discovered by E. Bowell on 1982 Jan 30 at Anderson Mesa station, which operated by Lowell Observatory. It is also known as 1982 BY1. We observed 1293 Sonja on two nights: 2016 Sep 6 and 9. We obtained a synodic period of 2.876 ± 0.001 h and an amplitude of 0.21 mag. References

Behrend, R. (2001, 2003, 2005, 2006, 2007, 2012, 2014). http://obswww.unige.ch/~behrend/page_cou.html

Benishek, V., Protitch-Benishek, V. (2008). “CCD Photometry of seven Asteroids at the Belgrade Astronomical Observatory.” Minor Planet Bul. 35, 28-30.

Benishek, V. (2015). “Rotation Period Determinations for 1724 Vladimir, 3965 Konopleva, and 9222 Chubey.” Minor Planet Bul. 42, 143-144.

Betzler, A.S., Ferreira, D.H., dos Santos, T.H.R., Novaes, A.B. (2008). “Lightcurve and Rotation Period of 1044 Teutonia.” Minor Planet Bul. 35, 26.

Binzel, R.P., Cochran, A.L., Barker, E.S., Tholen, D.J., Barucci, A., di Martino, M., Greenberg, R., Weidenschilling, S.J., Chapman, C.R., Davis, D.R. (1987a). “Coordinated Observations of asteroids 1219 Britta and 1972 Yi Xing.” Icarus 71, 148-158.

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Binzel, R.P. (1987b). “A photometric survey of 130 Asteroids.” Warner, B.D., Harris, A.W., Durech, J., Benner, L.A.M. (2016b). Icarus 72, 135-208. “Lightcurve Photometry Opportunities: July-September.” Minor Planet Bull. 43, 356-361. Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., 444 Gyptis.” Icarus 57, 251-258. Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Curves from the Palomar Transient Factory Survey: Rotation Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Periods and Phase Functions from Sparse Photometry.” Astron. J. H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, 150, A75. 24, 60, 261, and 863.” Icarus 77, 171-186.

Higgins, D., Goncalves, R.M.D. (2007). “Asteroid Lightcurve Analysis at Hunters Hill Observatory and Collaborating Stations - TARGET ASTEROIDS! OBSERVING CAMPAIGNS FOR June-September 2006.” Minor Planet Bul. 34, 16-18. JANUARY THROUGH MARCH 2017

Ivarsen, K., Willis, S., Ingleby, L., Matthews, D., Simet, M. Carl Hergenrother and Dolores Hill (2004). “CCD Observations and Period Determination of Fifteen Lunar & Planetary Laboratory Minor Planets.” Minor Planet Bul. 31, 29-33. University of Arizona 1629 E. University Blvd. JPL Small Body Database Search Engine. (2016). Tucson, AZ 85721 USA http://ssd.jpl.nasa.gov/sbdb_query.cgi [email protected]

Klinglesmith III, D.A., Hanowell, J., Risley, E., Turk, J., Vargas, (Received: 2016 October 15) A., Warren, C.A. (2014). “Lightcurves for Inversion Model Candidates.” Minor Planet Bul. 41, 139-143. Asteroid campaigns to be conducted by the Target Asteroids! program during the January-March 2017 Klinglesmith III, D.A., Franco, L. (2016). “Lightcurves for 1531 quarter are described. In addition to asteroids on the Hartmut and 4145 Maximova.” Minor Planet Bull. 43-2, 121. original Target Asteroids! list of easily accessible spacecraft targets, an effort has been made to identify Oey, J., Vilagi, J., Gajdos, S., Kornos, L., Galad, A. (2007). other asteroids that are 1) brighter and easier to observe “Light Curve Analysis of 8 Asteroids from Leura and other for small telescope users and 2) analogous to (101955) Collaborating Observatories.” Minor Planet Bul. 34, 81-83. Bennu and (162173) Ryugu, targets of the OSIRIS-REx and Hayabusa-2 sample return missions. Pravec, P., Wolf, M., Sarounova, L. (2008, 2012, 2015, 2016). http://www.asu.cas.cz/~ppravec/neo.htm Introduction Sada, P.V. (2008). “Lightcurve Analysis of 1084 Tamariwa.” Minor Planet Bul. 35, 50. The Target Asteroids! program strives to engage telescope users of all skill levels and telescope apertures to observe asteroids that are Sada, P.V., Navarro-Meza, S., Reyes-Ruiz, M., Olguin, L., viable targets for robotic sample return. The program also focuses Saucedo, J.C., Loera-Gonzalez, P. (2016). “Results of the 2015 on the study of asteroids that are analogous to (101955) Bennu Mexican Asteroid Photometry Campaign.” Minor Planet Bul. 43, and (162173) Ryugu, the target asteroids of the NASA OSIRIS- 154-156. REx and JAXA Hayabusa-2 sample return missions respectively. Most target asteroids are near-Earth asteroids (NEA) though Skiff, B.A. (2011). Posting on CALL web site. observations of relevant Main Belt asteroids (MBA) are also http://www.minorplanet.info/call.html requested. Stecher, G., Ford, L., Lorenzen, K., Ulrich, S. (2008). Even though many of the observable objects in this program are “Photometric Measurements of 1084 Tamariwa at Hobbs faint, acquiring a large number of low S/N observations allows Observatory.” Minor Planet Bul. 35, 76-77. many important parameters to be determined. For example, an Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid asteroid’s phase function can be measured by obtaining lightcurve database.” Icarus 202, 134-146. Updated 2016 Sep 6. photometry taken over a wide range of phase angles. The albedo http://www.MinorPlanet.info/lightcurvedatabase.html can be constrained from the phase angle observations, as there is a direct correlation between phase function and albedo (Belskaya Warner, B.D. (2014). “Asteroid Lightcurve Analysis at CS3- and Shevchenko 2000). The absolute magnitude can be estimated Palmer Divide Station: 2014 March-June.” Minor Planet Bul. 41, by extrapolating the phase function to a phase angle of 0°. By 157-168. combining the albedo and absolute magnitude, the size of the object can be estimated. Warner. B.D. (2015). MPO Canopus software. http://www.minorplanetobserver.com/MPOSoftware/ An overview of the Target Asteroids! program can be found at MPOCanopus.htm Hergenrother and Hill (2013).

Warner, B.D., Harris, A.W., Durech, J., Benner, L.A.M. (2016a). Current Campaigns “Lightcurve Photometry Opportunities: July-September.” Minor Planet Bull. 43, 278-281. Target Asteroids! continues to conduct a number of dedicated campaigns on select NEAs and analog carbonaceous MBAs Minor Planet Bulletin 44 (2017) 73 during the quarter. These campaigns have a primary goal of DATE RA DEC ∆ r V PH Elong conducting photometric measurements over a large range of phase 01/01 11 13 +06 14 2.71 3.23 14.3 16 113 angles. 01/11 11 13 +06 20 2.59 3.25 14.2 14 123 01/21 11 11 +06 40 2.49 3.26 14.1 12 134 01/31 11 07 +07 12 2.41 3.28 13.9 9 145 Target Asteroids! objects brighter than V = 17.0 are presented in 02/10 11 02 +07 55 2.36 3.29 13.7 6 157 detail. A short summary of our knowledge of each asteroid and 02/20 10 55 +08 44 2.33 3.31 13.5 3 169 10-day (shorter intervals for objects that warrant it) ephemerides 03/02 10 48 +09 34 2.33 3.32 13.3 0 177 are presented. The ephemerides include rough RA and Dec 03/12 10 40 +10 22 2.36 3.33 13.6 4 166 positions, distance from the Sun in AU (r), distance from Earth in 03/22 10 34 +11 03 2.42 3.35 13.8 7 154 AU (Δ), V magnitude, phase angle in degrees (PH) and elongation 04/01 10 28 +11 33 2.51 3.36 14.1 10 143 from the Sun in degrees (Elong). (379) Huenna (a=3.14 AU, e=0.19, i=1.7°, H = 8.9) We ask observers with access to large telescopes to attempt Similar to Erato, Huenna is also a member of the Themis family. It th observations of spacecraft accessible asteroids that are between V ranks as the 6 brightest Themis member at H = 8.9 (Nesvorny magnitude ~17.0 and ~20.0 during the quarter (contained in the 2015). Similar to other Themis objects, Huenna is carbonaceous table below). (B or C type) (Neese 2010).

Asteroid Peak V Time of Peak Huenna reaches a minimum phase angle of 0.6° and peak Number Name Mag Brightness brightness of V = 13.3 on February 28. It has a rotation period of (136635) 1994 VA1 18.7 early Feb 14.1 hours with a small amplitude of ~0.1 magnitudes (Behrend (141018) 2001 WC47 17.3 mid March 2014, Warner 2010). Both Huenna and Erato are located within a (163249) 2002 GT 19.6 early Jan (187040) 2005 JS108 19.4 early Jan few degrees of each other for the entire quarter providing an easy (433953) 1997 XR2 18.9 early Jan opportunity to observe two large Themis family objects during the night. Time series lightcurve and color photometry across a range The campaign targets are split up into two sections: carbonaceous of phase angles are requested. MBAs that are analogous to Bennu and Ryugu; and NEAs analogous to the Bennu and Ryugu or provide an opportunity to DATE RA DEC ∆ r V PH Elong fill some of the gaps in our knowledge of these spacecraft targets 01/01 11 13 +04 20 3.17 3.67 15.0 14 113 01/11 11 12 +04 23 3.04 3.68 14.9 12 123 (examples include very low and high phase angle observations, 01/21 11 10 +04 38 2.93 3.69 14.7 11 134 phase functions in different filters and color changes with phase 01/31 11 06 +05 04 2.83 3.69 14.6 8 145 angle). 02/10 11 01 +05 40 2.76 3.69 14.4 6 157 02/20 10 54 +06 24 2.72 3.69 14.2 2 169 The ephemerides listed below are just for planning purposes. In 03/02 10 47 +07 10 2.71 3.70 14.0 0 178 order to produce ephemerides for your observing location, date 03/12 10 40 +07 56 2.73 3.70 14.2 3 167 and time, please use the Minor Planet Center’s Minor Planet and 03/22 10 34 +08 38 2.78 3.70 14.4 6 155 Comet Ephemeris Service: 04/01 10 28 +09 13 2.85 3.71 14.6 9 144 http://www.minorplanetcenter.net/iau/MPEph/MPEph.html Near-Earth Asteroid Campaign Targets or the Target Asteroids! specific site created by Tomas Vorobjov (5604) 1992 FE (a=0.93 AU, e=0.41, i=4.7°, H = 17.2) and Sergio Foglia of the International Astronomical Search While most small asteroids are probably chips off a larger Collaboration (IASC) at asteroid, rarely can we say with much certainty that any near-Earth asteroid is a chip of a particular larger asteroid. In the case of V- http://iasc.scibuff.com/osiris-rex.php type NEA 1992 FE, it is highly likely that it is a piece of the main belt asteroid Vesta. Analog Carbonaceous Main Belt Asteroid Campaigns 1992 FE is an Aten NEA with an orbit that ranges from 0.55 to (62) Erato (a=3.13 AU, e=0.17, i=2.2°, H = 8.8) 1.31 AU from the Sun. This quarter 1992 FE passes within 0.034 Asteroid Erato is the 5th brightest member of the carbonaceous AU of Earth on February 24 with peak brightness occurring a few Themis family at H = 8.8 (Nesvorny 2015). The family’s days later on February 27 at V = 12.6 on February 27. It becomes namesake asteroid has been observed to have water ice and brighter than V = 17 on February 20 at a phase angle of 138°. It is organics on its surface (Campins et al. 2010, Rivkin and Emery not an easy object for northern observers until March 3 when it 2010). Some members also exhibit cometary activity confirming will still be V = 13. Minimum phase angle occurs on March 14 at the presence of ices. 37°.

Erato reaches a minimum phase angle of 0.1° and peak brightness In addition to its V-type taxonomy, we also know that 1992 FE is of V = 13.9 on March 1. Maximum phase angle occurs in late May a high-albedo object (0.53), roughly 1 km in diameter and has a at 17.1°. It is a Ch or B type asteroid with a rotation period of 9.2 rotation period of either 5.34 or 6.03 h with a moderate lightcurve hours and a small amplitude of ~0.15 magnitudes (Hanus et al. amplitude of 0.1-0.3 magnitudes (Bembrick and Pereghy 2003, 2011, Harris et al. 2015, Neese 2010). Time series lightcurve and Binzel et al. 2004, Higgins and Warner 2009, Koehn et al. 2014, color photometry across a range of phase angles are requested. Thomas et al. 2014, Ye et al. 2011). Time series lightcurve and color photometry across a range of phase angles are requested.

Minor Planet Bulletin 44 (2017) 74

DATE RA DEC ∆ r V PH Elong Koehn, B.W., Bowell, E.G., Skiff, B.A, Sanborn, J.J., McLelland, 02/20 22 24 -50 54 0.04 0.95 17.0 138 40 K.P., Pravec, P., Warner, B.D. (2014). “Lowell Observatory Near- 03/02 08 21 -33 49 0.05 1.02 12.8 52 125 Earth Asteroid Photometric Survey (NEAPS) – 2009 January 03/12 08 54 -11 25 0.11 1.08 14.2 37 138 through 2009 June”. Minor Planet Bulletin 41, 286-300. 03/22 09 07 -04 48 0.18 1.13 15.4 38 135 04/01 09 18 -01 47 0.26 1.18 16.3 41 129 Neese, C. (2010). “Asteroid Taxonomy V6.0”. EAR-A-5-DDR- (143404) 2003 BD44 (a=1.97 AU, e=0.61, i=2.7°, H = 16.8) TAXONOMY-V6.0”. NASA Planetary Data System. Little is known about 2003 BD44 other than its Apollo type orbit Nesvorny, D. (2015). “Nesvorny HCM Asteroid Families V3.0”. that takes it from 0.77 to 3.16 AU from the Sun. On March 20, it EAR-A-VARGBDET-5-NESVORNYFAM-V3.0. NASA passes through opposition and reaches a very low phase angle of Planetary Data System. 0.3°. It will remain bright for a few weeks after opposition as it peaks at V = 13.3 on April 12 and passes within 0.056 AU of Rivkin, A.S., Emery, J.P. (2010). "Detection of ice and organics Earth on April 18. The asteroid finally fades below V = 17 on on an asteroidal surface". Nature 464, 1322–1323. April 22 when it phase angle will reach over 130°. Time series lightcurve and color photometry across a range of phase angles are Thomas, C.A. et al. (2014). “Physical characterization of Warm requested. Spitzer-observed near-Earth objects”. Icarus 228, 217-246.

DATE RA DEC ∆ r V PH Elong Warner, B.D. (2010). “Asteroid Lightcurve Analysis at the Palmer 01/31 12 02 -02 42 0.87 1.68 18.9 26 129 Divide Observatory: 2009 December – 2010 March”. Minor 02/10 12 07 -03 17 0.72 1.60 18.3 24 138 Planet Bul. 37, 112-118. 02/20 12 11 -03 31 0.58 1.51 17.5 20 147 03/02 12 11 -03 12 0.45 1.42 16.7 15 157 Ye, Q. (2011). “BVRI photometry of 53 unusual asteroids”. 03/12 12 06 -02 05 0.34 1.33 15.7 8 169 03/22 11 55 +00 25 0.24 1.23 14.4 2 177 Astron. J. 141, 32. 04/01 11 30 +05 54 0.15 1.14 14.0 17 159

References LIGHTCURVE PHOTOMETRY OPPORTUNITIES: Behrend, R. (2014) Observatoire de Geneve website, 2017 JANUARY-MARCH http://obswww.unige.ch/~behrend/page_cou.html Brian D. Warner Belskaya, I., Shevchenko, V. (2000). “The Opposition Effect of Center for Solar System Studies / MoreData! Asteroids.” Icarus 147, 94-105. 446 Sycamore Ave. Eaton, CO 80615 USA Bembrick, C., Pereghy, B. (2003). “A period determination for the [email protected] Aten asteroid (5604) 1992 FE”. Minor Planet Bulletin 30, 43-44. Alan W. Harris Binzel, R.P. et al. (2004). “Observed Spectral Properties of Near- MoreData! Earth Objects: Results for Population Distribution, Source La Cañada, CA 91011-3364 USA Regions, and Space Weathering Processes”. Icarus 170, 259-294. Josef Ďurech Campins, H., Hargrove, K., Pinilla-Alonso, N., Howell, E.S., Astronomical Institute Kelley, M.S., Licandro, J., Mothé-Diniz, T., Fernández, Y., Ziffer, Charles University in Prague J. (2010). "Water Ice and Organics on the Surface of the Asteroid 18000 Prague, CZECH REPUBLIC 24 Themis". Nature 464, 1320–1321. [email protected]

Hanus, J., Durech, J., Broz, M., Warner, B.D., Pilcher, F., Lance A.M. Benner Stephens, R., Oey, J., Bernasconi, L., Casulli, S., Behrend, R., Jet Propulsion Laboratory Polishook, D., Henych, T., Lehky, M., Yoshida, F., Ito. T. (2011). Pasadena, CA 91109-8099 USA “A Study of Asteroid Pole-Latitude Distribution Based on an [email protected] Extended Set of Shape Models Derived by the Lightcurve Inversion Method”. Astron. Astrophys. 530, A134. We present lists of asteroid photometry opportunities for objects reaching a favorable apparition and have no or Harris, A.W., Warner, B.D., Pravec, P. (2015). “Asteroid poorly-defined lightcurve parameters. Additional data Lightcurve Derived Data V15.0”. EAR-A-5-DDR-DERIVED- on these objects will help with shape and spin axis LIGHTCURVE-V15.0. NASA Planetary Data System. modeling via lightcurve inversion. We also include lists of objects that will be the target of radar observations. Hergenrother, C., Hill, D. (2013). “The OSIRIS-REx Target Lightcurves for these objects can help constrain pole Asteroids! Project: A Small Telescope Initiative to Characterize solutions and/or remove rotation period ambiguities that Potential Spacecraft Mission Target Asteroids.” Minor Planet might not come from using radar data alone. Bulletin 40, 164-166.

Higgins D., Warner, B.D. (2009). “Lightcurve Analysis at Hunters We present several lists of asteroids that are prime targets for Hill Observatory and Collaborating Stations - Autumn 2009”. photometry during the period 2017 January-March. Minor Planet Bulletin 36, 159-160. 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

Minor Planet Bulletin 44 (2017) 75 base (LCDB; Warner et al., 2009) documentation for an Brightest LCDB Data Number Name Date Mag Dec Period Amp U explanation of the U code: ------31782 1999 KM6 01 20.2 15.6 +23 http://www.minorplanet.info/lightcurvedatabase.html 27675 1981 CH 01 20.4 15.4 +38 33349 1998 XF72 01 20.4 15.9 +30 13628 1995 WE 01 21.7 15.7 +31 The ephemeris generator on the CALL web site allows you to 2405 Welch 01 22.0 15.6 +19 12352 Jepejacobsen 01 22.6 15.4 +22 13.3954 0.42 2 create custom lists for objects reaching V ≤ 18.5 during any month 8126 Chanwainam 01 22.9 15.6 +19 in the current year, e.g., limiting the results by magnitude and 18429 1994 AO1 01 23.0 15.3 +14 declination. 1218 Aster 01 23.1 15.0 +25 5761 Andreivanov 01 24.1 15.5 +31 11.68 0.82-0.85 2 739 Mandeville 01 26.4 11.7 +12 11.931 0.14 2 http://www.minorplanet.info/PHP/call_OppLCDBQuery.php 27185 1999 CH37 01 26.9 16.0 +16 3.1546 0.25 2 4283 Stoffler 01 27.9 14.8 +38 136. 0.1-0.65 2- 2928 Epstein 01 29.4 15.2 +18 8.5088 0.37 2 We refer you to past articles, e.g., Minor Planet Bulletin 36, 188, 3569 Kumon 01 29.5 15.1 +5 for more detailed discussions about the individual lists and points 17065 1999 GK17 01 29.7 15.9 +17 of advice regarding observations for objects in each list. 5267 1966 CF 01 29.9 15.6 +22 22092 2000 AQ199 02 02.2 15.9 +15 18.8544 0.35 2 4099 Wiggins 02 06.1 15.5 +16 Once you’ve obtained and analyzed your data, it’s important to 5641 McCleese 02 09.2 15.1 +4 418. 0.06- 1.3 2 17591 1995 DG 02 12.0 15.9 +11 6.5577 0.37 2 publish your results. Papers appearing in the Minor Planet Bulletin 7811 Zhaojiuzhang 02 15.2 16.0 +22 3.3539 0.62-0.67 2 are indexed in the Astrophysical Data System (ADS) and so can 2916 Voronveliya 02 16.3 15.4 +10 be referenced by others in subsequent papers. It’s also important to 10263 Vadimsimona 02 17.2 15.5 -3 26421 1999 XP113 02 21.8 15.9 +7 make the data available at least on a personal website or upon 8212 Naoshigetani 02 23.6 15.4 +15 request. We urge you to consider submitting your raw data to the 3983 Sakiko 03 01.6 15.0 +7 10.5103 0.69 2 2546 Libitina 03 06.3 14.1 -3 132.71 0.35 2+ ALCDEF page on the Minor Planet Center web site: 18889 2000 CC28 03 07.0 16.0 +18 1910 Mikhailov 03 08.7 15.4 -3 8.88 0.25 2 http://www.minorplanetcenter.net/light_curve 3316 Herzberg 03 12.7 15.6 -2 9.6 0.1 1 4404 Enirac 03 15.6 15.0 +32 2.998 0.27 2+ 9148 Boriszaitsev 03 16.4 15.5 +2 We believe this to be the largest publicly available database of raw 3580 Avery 03 21.2 15.0 -2 24.2257 0.17-0.33 2 lightcurve data that contains 2.5 million observations for more 7421 Kusaka 03 22.4 16.0 -3 96.5 0.58-0.70 2 56116 1999 CZ7 03 22.5 15.3 -12 than 11500 objects. 138404 2000 HA24 03 25.8 15.6 -38 1969 Alain 03 26.3 15.1 -4 Now that many backyard astronomers and small colleges have 3748 Tatum 03 26.3 14.9 +2 58.21 0.54 2+ 6349 Acapulco 03 27.8 15.1 -14 4.3755 0.18 2 access to larger telescopes, we have expanded the photometry 2504 Gaviola 03 28.4 14.9 -3 8.7508 0.28 2 opportunities and spin axis lists to include asteroids reaching 2142 Landau 03 29.2 15.5 -3 V = 15.5 or brighter. 19743 2000 AF164 03 29.2 15.8 +15

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 Low Phase Angle Opportunities particularly favorable apparition. To keep the number of objects The Low Phase Angle list includes asteroids that reach very low manageable, the opportunities list includes only those objects reaching a particularly favorable apparition, meaning they could phase angles. The “α” column is the minimum solar phase angle all be set in bold text. for the asteroid. Getting accurate, calibrated measurements (usually V band) at or very near the day of opposition can provide Lightcurve/Photometry Opportunities important information for those studying the “opposition effect.” Objects with U = 3– or 3 are excluded from this list since they will Use the on-line query form for the LCDB likely appear in the list below for shape and spin axis modeling. Those asteroids rated U = 1 should be given higher priority over http://www.minorplanet.info/PHP/call_OppLCDBQuery.php those rated U = 2 or 2+, but not necessarily over those with no to get more details about a specific asteroid. period. On the other hand, do not overlook asteroids with U = 2/2+ on the assumption that the period is sufficiently established. You will have the best chance of success working objects with low Regardless, do not let the existing period influence your analysis amplitude and periods that allow covering at least half a cycle since even high quality ratings have been proven wrong at times. every night. Objects with large amplitudes and/or long periods are Note that the lightcurve amplitude in the tables could be more or much more difficult for phase angle studies since, for proper less than what’s given. Use the listing only as a guide. analysis, the data must be reduced to the average magnitude of the Brightest LCDB Data asteroid for each night. This reduction requires that you determine Number Name Date Mag Dec Period Amp U the period and the amplitude of the lightcurve; for long period ------objects that can be difficult. Refer to Harris et al. (1989; Icarus 13244 Dannymeyer 01 03.0 16.0 +24 88500 2001 QZ138 01 03.7 15.9 +25 81, 365-374) for the details of the analysis procedure. 12193 1979 EL 01 04.1 14.9 +29 8.9918 0.35 2 3931 Batten 01 04.3 16.0 +28 5399 Awa 01 05.1 14.9 +21 As an aside, some use the maximum light to find the phase slope 6117 1985 CZ1 01 06.8 15.6 +26 parameter (G). However, this can produce a significantly different 1674 Groeneveld 01 09.0 14.7 +23 8.1 0.19 2 value for both H and G versus when using average light, which is 2886 Tinkaping 01 09.0 14.8 +22 12. 0.13 1 1558 Jarnefelt 01 10.9 14.6 +22 18.22 0.40 2 the method used for values listed by the Minor Planet Center. 106589 2000 WN107 01 14.2 15.0 -63 47223 1999 VW10 01 14.6 15.7 +22 The International Astronomical Union (IAU) has adopted a new 45878 2000 WX29 01 15.8 15.4 +22 16.07 0.05 2 5693 1993 EA 01 16.3 15.4 +24 2.497 0.10 2 system, H-G12, introduced by Muinonen et al. (2010; Icarus 209, 1477 Bonsdorffia 01 16.7 14.9 +31 7.8 0.32 2 542-555). However it will be some years before it becomes the 4052 Crovisier 01 17.1 15.7 +23 Minor Planet Bulletin 44 (2017) 76 general standard and, furthermore, it is still in need of refinement. existing models, visit the Database of Asteroid Models from That can be done mostly through having more data for more Inversion Techniques (DAMIT) web site asteroids, but only if there are data at very low and moderate phase angles. Therefore, we strongly encourage observers to obtain data http://astro.troja.mff.cuni.cz/projects/asteroids3D for these objects not only at very low phase angles, but to follow them well before and/or after opposition, i.e., out to phase angles An additional dense lightcurve, along with sparse data, could lead of 15-30 degrees. to the asteroid being added to or improving one in DAMIT, thus increasing the total number of asteroids with spin axis and shape Num Name Date α V Dec Period Amp U models. ------500 Selinur 01 01.0 0.99 12.5 +26 8.011 0.10-0.16 3 514 Armida 01 02.3 0.43 13.1 +22 21.851 0.16-0.42 3 Included in the list below are objects that: 5399 Awa 01 05.1 0.67 15.0 +21 586 Thekla 01 06.0 0.71 13.0 +20 13.670 0.22-0.30 3 1. Are rated U = 3– or 3 in the LCDB 846 Lipperta 01 06.5 0.16 14.0 +22 1641. 0.30 2 861 Aida 01 07.2 0.46 14.4 +21 10.95 0.32 3 2. Do not have reported pole in the LCDB Summary table 561 Ingwelde 01 08.9 0.65 14.9 +20 12.012 0.38 3 2886 Tinkaping 01 09.0 0.03 14.8 +22 12. 0.13 1 3. Have at least three entries in the Details table of the LCDB 662 Newtonia 01 09.1 0.81 14.5 +20 21.095 0.42 3- where the lightcurve is rated U ≥ 2. 2410 Morrison 01 10.1 0.57 14.9 +21 215 Oenone 01 10.4 0.90 13.1 +24 27.937 0.18-0.20 3 1558 Jarnefelt 01 10.9 0.08 14.6 +22 18.22 0.40 2 The caveat for condition #3 is that no check was made to see if the 1847 Stobbe 01 11.3 0.50 14.4 +23 5.617 0.27-0.35 3 lightcurves are from the same apparition or if the phase angle 21 Lutetia 01 11.9 0.89 10.9 +24 8.166 0.06-0.25 3 158 Koronis 01 14.7 0.20 12.8 +21 14.218 0.28-0.43 3 bisector longitudes differ significantly from the upcoming 1623 Vivian 01 14.8 0.13 14.8 +21 20.521 0.85 3- apparition. The last check is often not possible because the LCDB 415 Palatia 01 21.3 0.69 11.4 +18 20.73 0.33 3 1398 Donnera 01 23.4 0.57 14.7 +18 7.231 0.15-0.26 3 does not list the approximate date of observations for all details 212 Medea 01 25.7 0.30 12.2 +20 10.283 0.03-0.16 3 records. Including that information is an on-going project. 299 Thora 01 26.9 0.99 14.2 +16 274. 0.39 2+ 54 Alexandra 01 30.8 0.25 12.0 +18 7.024 0.10-0.31 3 Brightest LCDB Data 472 Roma 01 30.9 0.75 11.8 +19 9.801 0.27-0.45 3 Num Name Date Mag Dec Period Amp U 406 Erna 02 03.1 0.07 14.8 +17 8.789 0.35 3 ------177 Irma 02 04.0 0.40 13.2 +17 13.856 0.24-0.37 3 514 Armida 01 02.3 13.1 +22 21.851 0.16-0.27 3 1128 Astrid 02 04.0 0.51 14.7 +18 10.228 0.29 2+ 586 Thekla 01 06.0 13.0 +20 13.67 0.24-0.30 3 1334 Lundmarka 02 07.0 0.48 14.4 +17 6.250 0.70 3- 4179 Toutatis 01 06.4 14.9 +11 176. 0.16-1.46 3 13276 1998 QP40 02 07.3 0.24 15.7 +16 530 Turandot 01 08.6 14.4 +18 19.96 0.10-0.16 3- 634 Ute 02 08.2 0.52 14.6 +17 11.755 0.14-0.17 3 2241 Alcathous 01 08.9 15.5 +15 7.689 0.20-0.34 3 103 Hera 02 10.3 0.28 11.5 +15 23.740 0.35-0.45 3 1806 Derice 01 10.6 13.7 +19 3.224 0.07-0.19 3 203 Pompeja 02 10.5 0.79 12.3 +16 24.052 0.10 3 206 Hersilia 01 11.9 12.1 +18 11.122 0.13-0.20 3 1252 Celestia 02 11.1 0.79 13.5 +16 10.636 0.26 3 1313 Berna 01 11.9 14.4 +24 25.46 0.20-0.28 3 2892 Filipenko 02 12.2 0.49 14.3 +15 14.00 0.21 3 855 Newcombia 01 14.4 15.5 +38 3.003 0.33-0.41 3 924 Toni 02 13.8 0.39 13.7 +12 19.437 0.1 -0.24 3 1117 Reginita 01 17.5 15.2 +17 2.946 0.10-0.33 3 2911 Miahelena 02 18.1 0.08 15.0 +12 4.201 0.56-0.66 3 2006 Polonskaya 01 17.5 15.5 +28 3.1183 0.08-0.16 3 1999 Hirayama 02 18.9 0.27 14.5 +12 15.63 0.45-0.57 3- 1866 Sisyphus 01 17.9 14.5 -33 2.4 0.01-0.14 3 1641 Tana 02 23.6 0.25 15.0 +09 7.95 0.32-0.33 3- 4440 Tchantches 01 17.9 15.0 +7 2.7883 0.21-0.34 3 62 Erato 02 28.7 0.54 13.3 +09 9.221 0.12-0.17 3 5143 Heracles 01 17.9 14.5 -27 2.7063 0.05-0.20 3 379 Huenna 03 01.4 0.16 13.9 +07 14.141 0.07-0.12 3 143 Adria 01 22.2 13.0 +29 22.005 0.07-0.10 3 243 Ida 03 02.8 0.21 13.6 +07 4.634 0.40-0.86 3 759 Vinifera 01 23.4 15.0 +27 14.229 0.36-0.40 3 269 Justitia 03 02.9 0.30 13.2 +08 33.128 0.14-0.25 3 1152 Pawona 01 24.5 13.8 +23 3.4154 0.16-0.26 3 16 Psyche 03 03.2 0.30 10.3 +08 4.196 0.03-0.42 3 235 Carolina 01 25.4 13.1 +30 17.61 0.30-0.38 3 1242 Zambesia 03 03.2 0.69 14.3 +09 15.72 0.15-1.36 2 3986 Rozhkovskij 01 26.1 14.6 +15 3.548 0.25-0.35 3 808 Merxia 03 08.3 0.68 13.0 +03 30.631 0.59-0.70 3 754 Malabar 01 27.5 13.6 -11 11.74 0.19-0.38 3 723 Hammonia 03 09.1 0.22 14.1 +05 5.436 0.18 3 1867 Deiphobus 01 28.9 15.4 +3 58.66 0.10-0.27 3- 1162 Larissa 03 10.9 0.51 14.7 +06 6.516 0.1 -0.20 3 472 Roma 01 30.8 11.8 +19 9.8007 0.27-0.45 3 289 Nenetta 03 11.2 0.56 14.2 +02 6.902 0.11-0.19 3 380 Fiducia 02 02.1 13.5 +22 13.69 0.04-0.32 3 672 Astarte 03 12.5 0.92 15.0 +01 22.572 0.10-0.17 3 266 Aline 02 03.5 13.1 -3 13.018 0.07-0.10 3 1636 Porter 03 12.9 0.22 14.9 +04 2.966 0.22-0.24 3 177 Irma 02 03.9 13.2 +17 13.856 0.24-0.37 3 109 Felicitas 03 15.1 0.66 12.4 +04 13.191 0.06-0.12 3 929 Algunde 02 04.5 14.4 +10 3.3102 0.13-0.19 3 635 Vundtia 03 16.1 0.65 13.5 +00 11.790 0.15-0.27 3 785 Zwetana 02 06.4 12.4 +35 8.8882 0.13-0.20 3 589 Croatia 03 16.9 0.12 13.4 +01 24.821 0.16-0.25 2+ 2448 Sholokhov 02 06.6 14.2 +19 10.061 0.21-0.63 3- 192 Nausikaa 03 18.3 0.86 11.1 -01 13.625 0.15-0.40 3 74 Galatea 02 07.5 12.9 +10 17.268 0.08-0.16 3 356 Liguria 03 20.1 0.37 11.8 -01 31.82 0.22 3- 971 Alsatia 02 08.6 13.2 +33 9.614 0.17-0.29 3 150 Nuwa 03 20.8 0.41 12.8 -01 8.135 0.08-0.31 3 5407 1992 AX 02 10.3 14.7 +25 2.5488 0.10-0.12 3 450 Brigitta 03 23.5 0.90 14.7 +02 10.766 0.18-0.30 3 6602 Gilclark 02 10.7 15.5 +32 4.5686 0.21-0.54 3 2002 Euler 03 24.2 0.57 14.9 +00 5.993 0.18-0.31 3 156 Xanthippe 02 11.8 12.0 +0 22.37 0.10-0.12 3 253 Mathilde 03 25.4 0.29 14.6 -01 417.7 0.45-0.50 3 3332 Raksha 02 14.0 14.5 +16 4.8065 0.25-0.36 3 1990 Pilcher 03 25.9 0.44 15.0 -03 1602 Indiana 02 15.3 14.4 +20 2.601 0.12-0.19 3 1462 Zamenhof 03 26.3 0.21 14.8 -02 10.4 0.15-0.30 2 40267 1999 GJ4 02 17.5 15.3 +14 4.9567 0.67-1.11 3 570 Kythera 03 26.8 0.39 14.1 -04 8.120 0.15-0.20 2 1257 Mora 02 17.8 15.0 +6 5.2948 0.23-0.43 3 119 Althaea 03 27.5 0.94 12.1 -05 11.484 0.23-0.36 3 504 Cora 02 18.1 14.7 +24 7.588 0.15-0.27 3- 952 Caia 03 27.8 0.75 14.5 +00 7.51 0.03-0.13 2 2911 Miahelena 02 18.1 14.9 +12 4.201 0.56-0.69 3 2504 Gaviola 03 28.4 0.20 14.9 -03 8.751 0.28 2 1999 Hirayama 02 18.9 14.4 +12 15.63 0.45-0.57 3- 77 Frigga 03 28.5 0.21 12.2 -03 9.012 0.07-0.20 3 3028 Zhangguoxi 02 19.6 14.8 +3 4.826 0.12-0.25 3 1512 Oulu 03 29.6 0.13 14.6 -03 132.3 0.33 2+ 275 Sapientia 02 21.7 11.5 +13 14.931 0.05-0.12 3- 1029 La Plata 03 30.1 0.47 14.5 -02 15.310 0.26-0.58 3 2478 Tokai 02 23.4 14.5 +3 25.885 0.41-0.90 3 533 Sara 03 31.6 0.65 13.4 -03 11.654 0.19-0.30 3 1829 Dawson 02 24.2 14.8 +2 4.254 0.05-0.28 3 5405 Neverland 03 31.8 0.57 15.0 -03 3.181 0.20 2 618 Elfriede 02 24.6 13.3 +25 14.795 0.12-0.17 3- 5605 Kushida 03 31.9 0.09 15.0 -05 517 Edith 02 24.7 13.7 +5 9.2747 0.08-0.18 3 947 Monterosa 02 25.8 14.2 +17 5.164 0.15-0.23 3- 5604 1992 FE 02 27.9 12.5 -47 5.3375 0.10-0.15 3 204 Kallisto 03 01.1 12.5 -1 19.489 0.09-0.26 3 Shape/Spin Modeling Opportunities 1520 Imatra 03 02.4 15.3 -13 18.635 0.27-0.35 3- 373 Melusina 03 02.5 14.2 +15 12.97 0.20-0.25 3 Those doing work for modeling should contact Josef Ďurech at the 1115 Sabauda 03 04.3 13.5 +28 6.75 0.16-0.27 3- 5448 Siebold 03 04.3 14.2 +3 2.9546 0.31-0.53 3 email address above. If looking to add lightcurves for objects with 1425 Tuorla 03 07.4 14.1 -2 7.75 0.17-0.40 3 713 Luscinia 03 07.8 14.6 -5 9.9143 0.09-0.40 3

Minor Planet Bulletin 44 (2017) 77 Brightest LCDB Data About YORP Acceleration Num Name Date Mag Dec Period Amp U ------33 Polyhymnia 03 10.1 13.8 +5 18.608 0.13-0.21 3 Many, if not all, of the targets in this section are near-Earth 252 Clementina 03 10.6 14.5 -3 10.864 0.32-0.44 3 asteroids. These objects are particularly sensitive to YORP 6170 Levasseur 03 11.0 14.7 +22 2.6529 0.09-0.14 3 289 Nenetta 03 11.2 14.2 +2 6.902 0.11-0.19 3 acceleration. YORP (Yarkovsky–O'Keefe–Radzievskii–Paddack) 2577 Litva 03 13.6 14.3 -5 2.8126 0.14-0.36 3 is the asymmetric thermal re-radiation of sunlight that can cause 635 Vundtia 03 16.1 13.5 +0 11.79 0.15-0.27 3 348 May 03 16.9 13.6 +15 7.3812 0.14-0.16 3 an asteroid’s rotation period to increase or decrease. High 3712 Kraft 03 17.3 15.2 -51 9.341 0.27-1.20 3 precision lightcurves at multiple apparitions can be used to model 1052 Belgica 03 18.3 15.1 +8 2.7097 0.08-0.10 3 the asteroid’s sidereal rotation period and see if it’s changing. 70 Panopaea 03 19.0 12.1 +14 15.808 0.07-0.14 3- 309 Fraternitas 03 19.7 14.2 +0 22.398 0.10-0.35 3 5333 Kanaya 03 21.8 14.9 -10 3.8022 0.15-0.22 3 It usually takes four apparitions to have sufficient data to 1171 Rusthawelia 03 23.7 14.8 +2 10.98 0.26-0.31 3 determine if the asteroid rotation rate is changing under the 4374 Tadamori 03 23.8 14.9 +3 4.5047 0.77-0.94 3 198 Ampella 03 25.9 12.7 -14 10.379 0.03-0.22 3 influence of YORP. So, while obtaining a lightcurve at the current 811 Nauheima 03 26.4 14.8 +1 4.0011 0.08-0.20 3 apparition may not result in immediately seeing a change, the data 240 Vanadis 03 30.1 13.0 -1 10.64 0.13-0.34 3 1029 La Plata 03 30.1 14.5 -2 15.31 0.26-0.58 3 are still critical in reaching a final determination. This is why 782 Montefiore 03 30.3 13.5 +5 4.0728 0.42-0.54 3 observing asteroids that already have well-known periods can still 533 Sara 03 31.6 13.3 -3 11.654 0.19-0.30 3 be a valuable use of telescope time. It is even more so when considering BYORP (binary-YORP) among binary asteroids where that effect has stabilized the spin so that acceleration of the Radar-Optical Opportunities primary body is not the same as if it would be if there were no There are several resources to help plan observations in support of satellite. radar. Name Grp Period App Last Bin R SNR Future radar targets: 2003 UX34 NEA - - - - 71 G http://echo.jpl.nasa.gov/~lance/future.radar.nea.periods.html Tantalus NEA 2.384 2 2014 ? 10 G Past radar targets: 1999 JV6 NEA 6.838 3 2016 - 394 A http://echo.jpl.nasa.gov/~lance/radar.nea.periods.html 1998 XB NEA 500. 1 2005 - 335 G 2010 LN14 NEA - - - - 291 A Arecibo targets: http://www.naic.edu/~pradar/sched.shtml 2005 EE NEA - - - - 155 A http://www.naic.edu/~pradar 1999 VG22 NEA - - - - 35 A Toutatis NEA 176 6 2013 - 3000 G Goldstone targets: 2003 BD44 NEA - - - - 2000 A http://echo.jpl.nasa.gov/asteroids/goldstone_asteroid_schedule.html 1991 VK NEA 4.21 2 2016 - 37 G However, these are based on known targets at the time the list was 2013 WT67 NEA 135. 1 2014 - 1140 A prepared. It is very common for newly discovered objects to move 1998 QK56 NEA 9.84 1 2016 - 192 A up the list and become radar targets on short notice. We 1992 FE NEA 5.338 2 2009 - 2500 G recommend that you keep up with the latest discoveries the Minor 2000 HA24 NEA - - - - 42 G Planet Center observing tools 2003 HF2 NEA - - - - 3400 A In particular, monitor NEAs and be flexible with your observing Table I. Summary of radar-optical opportunities in 2017 Jan-Mar. program. In some cases, you may have only 1-3 days when the Data from the asteroid lightcurve database (Warner et al., 2009; Icarus 202, 134-146). asteroid is within reach of your equipment. Be sure to keep in touch with the radar team (through Dr. Benner’s email listed To help focus efforts in YORP detection, Table I gives a quick above) if you get data. The team may not always be observing the summary of this quarter’s radar-optical targets. The Grp column target but your initial results may change their plans. In all cases, gives the family or group for the asteroid. The period is in hours your efforts are greatly appreciated. and, in the case of binary, for the primary. The App columns gives the number of different apparitions at which a lightcurve period Use the ephemerides below as a guide to your best chances for was reported while the Last column gives the year for the last observing, but remember that photometry may be possible before reported period. The Bin column is ‘Y’ if the asteroid has one or and/or after the ephemerides given below. Note that geocentric more satellites (a ‘?’ indicates a suspected binary). The last positions are given. Use these web sites to generate updated and column indicates the estimated radar SNR using the tool at topocentric positions: http://www.naic.edu/~eriverav/scripts/radarscript.php MPC: http://www.minorplanetcenter.net/iau/MPEph/MPEph.html JPL: http://ssd.jpl.nasa.gov/?horizons The estimate in Table I is based on using the Arecibo (A) or Goldstone (G) radar. Goldstone is the default if a close approach is In the ephemerides below, ED and SD are, respectively, the Earth outside the declination range of Arecibo. The estimate uses the and Sun distances (AU), V is the estimated Johnson V magnitude, current MPCORB absolute magnitude (H), a period of 3.0 hours if and α is the phase angle. SE and ME are the great circles distances it’s not known, and the approximate minimum Earth distance (in degrees) of the Sun and Moon from the asteroid. MP is the during the three-month period covered by this paper. lunar phase and GB is the galactic latitude. “PHA” indicates that the object is a “potentially hazardous asteroid”, meaning that at If the SNR value is in bold text, the object was found on the radar some (long distant) time, its orbit might take it very close to Earth. planning pages listed above. Otherwise, the search tool at

Minor Planet Bulletin 44 (2017) 78

http://www.minorplanet.info/PHP/call_OppLCDBQuery.php (96590) 1998 XB (Jan-Feb, H = 16.2) This asteroid has reported a period between 500-520 hours (Pravec was used to find known NEAs that were V < 18.0 during the et al., 2005). Given the somewhat large phase angle, the lightcurve quarter. An object was placed on the list only if the estimated may have some unusual features. A campaign of determined and radar SNR > 10. This would produce a very marginal signal, not well-coordinated observers is in order. The low galactic latitudes enough for imaging, but might allow improving orbital parameters could make this a difficult target. Remember to get a prolonged run of data throughout each night and not just a few random data (226514) 2003 UX34 (Dec-Jan, H = 20.0) points. This helps assure correctly finding the nightly trends as This NEA has an estimated diameter of about 300 meters. The well as to look for a short period component (see Warner, MPB rotation period has not yet been determined. Early January will 43, 306-309). provided the best opportunity for smaller backyard telescopes. DATE RA Dec ED SD V α SE ME MP GB DATE RA Dec ED SD V α SE ME MP GB ------01/01 02 21.7 +22 03 0.37 1.21 16.2 45.0 120 88 +0.07 -36 01/01 02 21.7 +22 03 0.37 1.21 16.2 45.0 120 88 +0.07 -36 01/11 02 27.1 +25 06 0.45 1.22 16.7 48.5 111 50 +0.97 -33 01/11 02 27.1 +25 06 0.45 1.22 16.7 48.5 111 50 +0.97 -33 01/21 02 37.4 +27 36 0.53 1.23 17.1 51.0 104 163 -0.40 -30 01/21 02 37.4 +27 36 0.53 1.23 17.1 51.0 104 163 -0.40 -30 01/31 02 51.4 +29 45 0.60 1.22 17.5 52.8 98 63 +0.10 -26 01/31 02 51.4 +29 45 0.60 1.22 17.5 52.8 98 63 +0.10 -26 02/10 03 08.4 +31 39 0.67 1.22 17.7 54.2 92 76 +0.99 -23 02/10 03 08.4 +31 39 0.67 1.22 17.7 54.2 92 76 +0.99 -23 02/20 03 27.9 +33 22 0.74 1.20 17.9 55.4 87 155 -0.39 -19 02/20 03 27.9 +33 22 0.74 1.20 17.9 55.4 87 155 -0.39 -19 03/02 03 49.5 +34 52 0.79 1.18 18.1 56.5 82 42 +0.14 -15 03/02 03 49.5 +34 52 0.79 1.18 18.1 56.5 82 42 +0.14 -15 03/12 04 13.2 +36 10 0.84 1.15 18.2 57.6 77 96 +1.00 -11 03/12 04 13.2 +36 10 0.84 1.15 18.2 57.6 77 96 +1.00 -11

(438955) 2010 LN14 (Jan-Feb, H = 21.1) 2102 Tantalus (Dec-Jan, Binary?, H = 16.5) The rotation period for this 180-meter NEA has not been Pravec et al. (1997) reported a period of 2.391 h. Warner (2015) determined. The size is on the edge of making this a likely super- reported a possible satellite based on a second period of about 16 fast rotator. Keep exposures as short as possible until preliminary hours in addition to a “primary” period of 2.384 h. High-quality analysis indicates a period. data (< 0.03 mag precision) will be needed to help confirm the satellite. DATE RA Dec ED SD V α SE ME MP GB ------01/15 13 38.2 +08 41 0.06 0.99 17.8 81.4 95 54 -0.92 +69 On the other hand, the lack of evidence (negative observations) 01/18 12 19.4 +15 21 0.06 1.02 17.3 58.4 118 16 -0.68 +76 will not automatically mean that the earlier analysis observations 01/21 11 12.9 +19 26 0.08 1.04 17.1 39.5 138 61 -0.40 +66 and analysis were incorrect. Favoring confirmation is that the 01/24 10 23.5 +21 25 0.09 1.07 17.2 25.5 152 107 -0.15 +56 01/27 09 48.3 +22 14 0.11 1.09 17.3 15.3 163 151 -0.01 +48 phase angle bisector longitude will be about 180° from the time 01/30 09 23.2 +22 30 0.13 1.11 17.5 8.1 171 161 +0.04 +43 Warner observed the NEA. This means that the viewing geometry 02/02 09 04.9 +22 31 0.15 1.14 17.7 4.9 174 117 +0.27 +39 of the purported satellite orbit will be about the same, the 02/05 08 51.4 +22 25 0.18 1.16 18.2 7.1 172 73 +0.60 +36 difference being, e.g., a view favoring the south pole of primary instead of its north pole. (265482) 2005 EE (Jan-Feb, H = 21.3) 2005 EE is an NEA with an estimated diameter of 160 meters. January is the best time to catch this. While still bright enough to This makes it another candidate for being a super-fast rotator. work into February and March, the galactic latitude is near 0°, put Because of the need for short exposures means larger scopes the asteroid in rich star fields. (0.5-m or more) are preferred. DATE RA Dec ED SD V α SE ME MP GB ------DATE RA Dec ED SD V α SE ME MP GB 01/01 02 11.4 -01 54 0.14 1.04 14.1 63.8 109 79 +0.07 -58 ------01/05 01 06.8 +18 19 0.17 1.02 14.8 72.7 98 22 +0.41 -44 01/20 13 45.6 +10 08 0.07 1.00 18.3 77.2 99 18 -0.49 +69 01/09 00 20.8 +30 06 0.22 1.00 15.5 78.2 89 52 +0.84 -32 01/23 13 14.2 +16 56 0.08 1.01 18.1 65.1 111 57 -0.23 +79 01/13 23 48.6 +36 36 0.28 0.99 16.1 80.6 83 105 -1.00 -25 01/26 12 45.0 +22 29 0.08 1.03 18.0 54.5 121 99 -0.04 +85 01/17 23 25.2 +40 26 0.35 0.97 16.5 81.2 78 135 -0.77 -20 01/29 12 18.4 +26 50 0.09 1.05 18.0 45.7 130 139 +0.01 +83 01/21 23 07.7 +42 51 0.42 0.96 16.8 80.7 75 123 -0.40 -16 02/01 11 54.3 +30 07 0.10 1.06 18.0 38.3 138 151 +0.17 +77 01/25 22 53.9 +44 28 0.48 0.95 17.1 79.7 72 91 -0.09 -14 02/04 11 32.8 +32 32 0.12 1.08 18.1 32.4 144 116 +0.48 +72 02/07 11 13.8 +34 14 0.13 1.10 18.3 27.9 149 74 +0.81 +68 01/29 22 42.8 +45 35 0.54 0.94 17.3 78.3 69 61 +0.01 -12 02/10 10 57.2 +35 24 0.14 1.11 18.4 24.6 152 36 +0.99 +64

(85990) 1999 JV6 (Jan, H = 20.2) (413002) 1999 VG22 (Jan-Mar, H = 18.7) Warner (2014, 2015, and 2016) has reported a period of about For radar observations, the relatively large size of 0.55 km for this 6.54 hours for this NEA. The primary goals for observations are NEA is countered by its Earth distance of more than 0.1 AU. The for lightcurve inversion modeling and building a longer time result is a low SNR. Still, photometric and astrometric frame to look for YORP influence in the coming years. observations will be helpful, especially the former. Expect a DATE RA Dec ED SD V α SE ME MP GB period greater than 2 hours. ------01/10 02 21.3 -11 39 0.07 1.00 17.2 77.6 98 49 +0.91 -64 DATE RA Dec ED SD V α SE ME MP GB 01/11 02 37.0 -08 19 0.07 1.00 17.1 73.6 102 58 +0.97 -59 ------01/12 02 51.5 -05 09 0.08 1.01 17.1 69.9 106 67 +1.00 -54 01/01 09 48.1 +08 27 0.20 1.13 17.0 38.6 134 165 +0.07 +43 01/13 03 04.9 -02 10 0.08 1.01 17.1 66.5 109 76 -1.00 -49 01/11 10 21.3 +01 56 0.18 1.12 16.8 39.5 134 65 +0.97 +46 01/14 03 17.3 +00 35 0.08 1.02 17.1 63.5 112 87 -0.97 -45 01/21 10 52.8 -04 49 0.17 1.11 16.6 40.2 133 58 -0.40 +47 01/15 03 28.7 +03 07 0.09 1.02 17.1 60.8 115 97 -0.92 -41 01/31 11 20.3 -10 57 0.16 1.10 16.5 39.9 134 163 +0.10 +46 01/16 03 39.2 +05 26 0.09 1.03 17.1 58.4 117 107 -0.85 -38 02/10 11 42.2 -15 44 0.16 1.11 16.5 37.9 136 55 +0.99 +44 01/17 03 48.9 +07 31 0.09 1.03 17.2 56.3 119 117 -0.77 -35 02/20 11 57.4 -18 50 0.17 1.12 16.5 33.9 141 70 -0.39 +42 03/02 12 05.9 -20 09 0.18 1.15 16.5 28.1 147 153 +0.14 +41 03/12 12 09.1 -19 54 0.19 1.17 16.5 21.3 155 32 +1.00 +42 03/22 12 09.5 -18 30 0.22 1.21 16.6 14.8 162 97 -0.37 +43 04/01 12 09.5 -16 29 0.25 1.24 16.9 11.5 166 122 +0.20 +45 Minor Planet Bulletin 44 (2017) 79

4179 Toutatis (Jan-Mar, NPAR (tumbler), H = 15.3) (443103) 2013 WT67 (Feb-Mar, H = 18.0) This well-studied asteroid is in non-principal axis rotation Warner (2015) found a period of 135 h with a possibility of (NPAR), commonly known as tumbling. The periods of rotation tumbling. A well-coordinated campaign involving observers from and precession are 176 and 130 h (Pravec et al., 2005). There are widely separated longitudes will be required to give this 750-m several radar generated “movies” showing the rotation of the NEA the attention it needs. asteroid, e.g., http://www.jpl.nasa.gov/video/details.php?id=1175. DATE RA Dec ED SD V α SE ME MP GB ------Period analysis of a tumbler requires specialized software such as 02/20 03 19.3 +11 47 0.11 0.97 16.6 94.0 79 156 -0.39 -37 that developed by Petr Pravec. Even so, because of the long 02/25 04 18.4 +00 21 0.13 0.99 16.5 86.0 87 106 -0.03 -33 periods involved, consideration should be given to a prolonged 03/02 05 03.2 -08 25 0.15 1.01 16.7 79.6 92 53 +0.14 -28 03/07 05 36.9 -14 30 0.18 1.02 16.9 74.9 95 36 +0.67 -23 campaign involving several observers at widely-spaced locations 03/12 06 02.9 -18 39 0.21 1.04 17.2 71.5 97 78 +1.00 -19 and a standardized method so that all data can be put onto a 03/17 06 23.9 -21 33 0.24 1.06 17.4 68.9 98 120 -0.82 -15 03/22 06 41.4 -23 37 0.27 1.07 17.7 66.8 99 137 -0.37 -13 common system (zero point), even if it’s only internal and not one 03/27 06 56.8 -25 07 0.31 1.09 17.9 65.2 99 107 -0.02 -10 such as the Johnson-Cousins system.

Try to catch this as soon into the New Year as possible. The (10636) 1998 QK56 (Feb-Mar, H = 17.6) galactic latitude decreases to near 0° while the magnitude Warner (2016) found a period 9.84 hours for 1998 QK56, an NEA increases, making the asteroid a more difficult target by Ground with an estimated diameter of 900 meters. Taking moon Hog Day. elongation and galactic latitude into account, early February and late March appear to provide the best opportunities. DATE RA Dec ED SD V α SE ME MP GB ------01/01 01 13.4 +06 33 0.25 1.05 14.9 67.4 99 68 +0.07 -56 DATE RA Dec ED SD V α SE ME MP GB 01/06 01 58.1 +11 01 0.26 1.08 14.9 60.8 106 14 +0.52 -49 ------01/11 02 40.8 +14 48 0.28 1.12 14.9 54.8 112 48 +0.97 -40 02/01 02 24.6 -38 11 0.23 0.94 17.6 93.7 73 48 +0.17 -68 01/16 03 19.7 +17 42 0.31 1.15 15.0 49.7 116 109 -0.85 -33 02/09 03 27.0 -37 01 0.18 0.97 17.0 88.8 81 81 +0.95 -56 01/21 03 54.1 +19 49 0.34 1.19 15.2 45.8 120 162 -0.40 -26 02/17 04 54.1 -31 45 0.15 1.01 16.2 77.0 95 126 -0.67 -38 01/26 04 23.9 +21 16 0.39 1.23 15.5 42.8 122 145 -0.04 -19 02/25 06 36.1 -19 20 0.14 1.06 15.5 58.1 115 129 -0.03 -12 01/31 04 49.7 +22 14 0.43 1.27 15.7 40.6 123 86 +0.10 -14 03/05 08 04.2 -03 54 0.15 1.10 15.3 39.9 134 57 +0.45 +14 02/05 05 12.3 +22 51 0.49 1.32 16.0 39.0 123 22 +0.60 -10 03/13 09 05.6 +07 13 0.20 1.16 15.7 30.8 143 42 -1.00 +33 03/21 09 46.6 +13 27 0.26 1.22 16.4 28.8 144 130 -0.47 +45 03/29 10 15.3 +16 40 0.33 1.27 17.0 29.5 141 129 +0.01 +52

(143404) 2003 BD44 (Feb-Apr, H = 16.6, PHA) No rotation period has been reported for this 1.3 km NEA. Follow (5604) 1992 FE (Mar, H = 17.2) this across as wide a range of phase angles as possible (e.g., once Bembrick et al. (2003) found a period of 6.02 h while Higgins et every 7-10 days), getting a complete lightcurve at every interval. al. (2009) and Koehn et al. (2014) found a period of about 5.3 This will allow finding more accurate values for H (absolute hours. Southern Hemisphere observers will have the best chance magnitude) and G (phase slope parameter). Be careful, however, to help remove any remaining uncertainties about the period. The of trying to merge the lightcurves into a single solution: the estimated size for this NEA is 1.1 km. synodic period and especially the shape of the lightcurve may evolve dramatically during the apparition. DATE RA Dec ED SD V α SE ME MP GB ------03/01 08 09.5 -40 22 0.05 1.01 12.6 58.0 120 107 +0.07 -4 DATE RA Dec ED SD V α SE ME MP GB 03/06 08 40.3 -21 15 0.07 1.05 13.3 41.9 135 61 +0.56 +12 ------03/11 08 52.1 -12 49 0.11 1.08 14.0 37.6 139 31 +0.97 +20 02/01 12 02.6 -02 46 0.87 1.68 18.8 26.5 130 175 +0.17 +58 03/16 08 59.6 -08 13 0.14 1.10 14.7 37.0 138 78 -0.89 +24 02/11 12 08.2 -03 20 0.71 1.60 18.2 24.0 139 41 +1.00 +58 03/21 09 05.7 -05 22 0.18 1.13 15.2 37.9 136 132 -0.47 +27 02/21 12 11.3 -03 31 0.57 1.51 17.5 20.2 148 83 -0.30 +58 03/26 09 11.4 -03 26 0.21 1.15 15.7 39.2 133 155 -0.06 +29 03/03 12 10.9 -03 10 0.45 1.42 16.6 14.8 159 144 +0.23 +58 03/31 09 17.1 -02 04 0.25 1.18 16.2 40.6 130 91 +0.12 +31 03/13 12 06.0 -01 57 0.33 1.32 15.6 7.4 170 6 -1.00 +59 04/05 09 23.1 -01 06 0.29 1.20 16.5 42.1 127 26 +0.64 +33 03/23 11 54.0 +00 42 0.24 1.23 14.4 3.2 176 120 -0.28 +60 04/02 11 28.0 +06 33 0.15 1.14 13.9 19.5 158 91 +0.30 +61 04/12 10 10.9 +22 43 0.08 1.05 13.3 52.6 124 64 -0.99 +54 (138404) 2000 HA24 (Mar-Apr, H = 19.1) The rotation period for 2000 HA24, a 500-meter NEA, has (7341) 1991 VK (Feb-Apr, H = 17.0) apparently not been reported. Late March and later will be the Pravec et al. (1998, A = 0.70 mag) and Warner (2016, A = 0.21 better time to observe the asteroid. It will still be relatively bright mag) each found a period of about 4.2 hours for this 1.4 km NEA. and farther away from the galactic plane. Warner observed at a phase angle bisector longitude of about 10°, or almost 180° from the longitude for this apparition. Expect, but DATE RA Dec ED SD V α SE ME MP GB don’t assume, an amplitude closer to 0.2 mag than 0.7 mag, ------03/15 16 56.7 -47 10 0.07 1.00 16.1 80.5 96 61 -0.94 -2 keeping in mind that amplitude increases with phase angle. 03/20 15 30.7 -44 04 0.08 1.03 15.7 60.9 115 36 -0.56 +10 03/25 14 30.3 -38 53 0.09 1.06 15.6 44.6 132 96 -0.12 +20 DATE RA Dec ED SD V α SE ME MP GB 03/30 13 50.0 -33 34 0.10 1.08 15.7 31.7 145 155 +0.05 +28 ------04/04 13 23.0 -28 52 0.12 1.11 15.8 21.8 156 101 +0.53 +34 02/01 12 02.6 -02 46 0.87 1.68 18.8 26.5 130 175 +0.17 +58 04/09 13 04.6 -24 57 0.14 1.14 16.0 15.4 162 36 +0.95 +38 02/11 12 08.2 -03 20 0.71 1.60 18.2 24.0 139 41 +1.00 +58 04/14 12 52.0 -21 45 0.16 1.16 16.3 13.1 165 39 -0.93 +41 02/21 12 11.3 -03 31 0.57 1.51 17.5 20.2 148 83 -0.30 +58 04/19 12 43.5 -19 11 0.19 1.19 16.7 14.7 163 97 -0.54 +44 03/03 12 10.9 -03 10 0.45 1.42 16.6 14.8 159 144 +0.23 +58 04/24 12 38.1 -17 08 0.22 1.21 17.1 17.9 158 159 -0.09 +46 03/13 12 06.0 -01 57 0.33 1.32 15.6 7.4 170 6 -1.00 +59 04/29 12 35.2 -15 31 0.25 1.23 17.6 21.4 153 118 +0.09 +47 03/23 11 54.0 +00 42 0.24 1.23 14.4 3.2 176 120 -0.28 +60 04/02 11 28.0 +06 33 0.15 1.14 13.9 19.5 158 91 +0.30 +61 04/12 10 10.9 +22 43 0.08 1.05 13.3 52.6 124 64 -0.99 +54 (215588) 2003 HF2 (Mar-Apr, H = 19.4)

This NEA has an estimated effective diameter of 390 meters, so its rotation period is very likely more than 2 hours. The first few days Minor Planet Bulletin 44 (2017) 80 of April will provide the best opportunity to find a rotation period. Because of the large phase angle, be careful about assuming a bimodal shape for the lightcurve, even the amplitude exceeds 0.5 mag.

DATE RA Dec ED SD V α SE ME MP GB ------03/30 06 41.7 +19 09 0.05 1.00 15.7 86.7 91 65 +0.05 +7 03/31 07 40.8 +18 40 0.05 1.01 15.6 73.6 104 64 +0.12 +19 04/01 08 25.1 +17 32 0.06 1.02 15.6 63.8 113 60 +0.20 +28 04/02 08 57.3 +16 18 0.07 1.04 15.7 56.7 120 53 +0.30 +35 04/03 09 21.0 +15 11 0.08 1.05 15.9 51.6 125 45 +0.42 +40 04/04 09 38.8 +14 14 0.09 1.06 16.1 47.9 128 35 +0.53 +43 04/05 09 52.6 +13 26 0.10 1.07 16.4 45.2 131 25 +0.64 +46 04/06 10 03.6 +12 46 0.12 1.08 16.6 43.1 132 14 +0.74 +48 04/07 10 12.4 +12 11 0.13 1.09 16.8 41.6 134 3 +0.83 +50 04/08 10 19.8 +11 42 0.14 1.10 17.0 40.3 134 8 +0.90 +51

Minor Planet Bulletin 44 (2017) 81

AUTHORS GUIDE were checked against the period of 10.45 h found by Smith (2010) but this produced an unconvincing fit.” The Minor Planet Bulletin (MPB) is open to papers on all aspects of minor planet study. Theoretical, observational, historical, Manuscript Submission review, and other topics from amateur and professional astronomers are welcome. The level of presentation should be All material should be submitted electronically to the Minor such as to be readily understood by most amateur astronomers. Planet Bulletin editor, Professor Richard Binzel: The preferred language is English. All observational and theoretical papers will be reviewed by another researcher prior to Dr. Richard Binzel publication to insure that results are presented clearly and MIT 54-410 concisely. Typically, papers will be published within three months 77 Massachusetts Ave. of receipt. However, material submitted on or before the posted Cambridge, MA 02139 USA deadline may or may not appear in that issue, depending on email: [email protected] available space and editorial processing. Manuscript Preparation There is no formal word or page count limit. Manuscripts should be as concise as possible but not to the point of sacrificing clarity Authors are asked to carefully comply with the guidelines below or accuracy. in order to minimize the time required for editorial tasks.

For lightcurve articles, authors are encouraged to combine as We strongly encourage that all submissions be made electronically many objects together in a single article as possible. When using MS Word or OpenOffice files (saved in MS Word format). presenting data on more than one asteroid, the asteroids should be If using Word 2007 or later, please save in DOCX instead of DOC listed in numerical order throughout, i.e., in the title, abstract, text format. body, and tables. Unnumbered asteroids should be listed after any It is strongly requested that all manuscripts be prepared using the numbered asteroids and by designation, which is – generally – the MS Word template found at: order of discovery. See recent MPB issues for examples. http://www.minorplanet.info/minorplanetbulletin.html The MPB will not generally publish articles on instrumentation. Persons interested in details of CCD instrumentation should Preferred Order consult web sites that provide both general information and specifics for given programs, such as: Most papers should follow this outline:

American Association of Variable Star Observers (AAVSO). 1. Title An excellent CCD photometry handbook can be found on this 2. Author list site. http://www.aavso.org 3. Abstract International Occultation Timing Association (IOTA). 4. Body Text http://www.lunar-occultations.com/iota/iotandx.htm Figures, e.g., lightcurves, can be embedded within the Astrometry measurements should be submitted to the IAU Minor body so that they are close to the text that discusses them. Planet Center http://minorplanetcenter.org/iau/mpc.html and are See more under “Figures.” no longer being published or reproduced in the MPB. The body text can contain a number of sections, as does this guide. Sections should be given a title using the Checking Previous Research Header 2 paragraph style. Generally, keep the number of sections to a minimum. For When reporting lightcurve results, authors should consult the example, it is not necessary, and even discouraged, to Astrophysics Data System (ADS, http://adsabs.harvard.edu/ create an “Introduction” section that leads into an abstract_service.html) and the Asteroid Lightcurve Database “Equipment” section followed by “Observations.” All of (LCDB; http://www.minorplanet.info/lightcurvedatabase.html) to these, unless there is a very specific reason otherwise, look for previous results on each object. If using the LCDB, your should go into the body text without section headers. reference to previous results should not be to the LCDB. Instead, your reference should be to the original author and publication 5. Standard Table (see below). where the currently accepted “best result” is reported, e.g. 6. Acknowledgements Lagerkvist (1978). 7. References Claims of priority: “These are the first lightcurves reported for 8. Figures, if not embedded in the body text. asteroid x.” is not an appropriate style for the Minor Planet Bulletin. Instead, something like: “A search of the Asteroid The abstract and body text should be written as if the other does Lightcurve Database (or other resources) did not find any not exist. Specifically, the first paragraph after the abstract should previously reported results for asteroid x.” is considered more not be a continuation of the abstract. It may, and often does, sound acceptable. redundant for the first paragraph to be a rephrasing of the abstract. Regardless, the two should be independent of one another. If previous results have been reported and they are different from yours (beyond the error margins), try fitting your data to those Tables other periods and report your “compare and contrast” results as The font size of a table’s contents should be large enough to allow part of the paper. This can be a brief statement, e.g., “The data for clear reproduction, usually no less than 6.5 points, preferably 8

Minor Planet Bulletin 44 (2017) 82

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Grp 1727 Mette 04/21-04/29 657 21.7,20.7 228 33 2.9812 0.0002 0.32 0.02 H 70030 Margaretmiller 05/09 245 24.3 268 -21

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. D a/b b/c 10306 Pagnol 07/16-08/01 163 5.9,5.6,7.7 298 11 4.79 0.01 0.27 0.05 9.1* 1.23 1.04 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle values are for the first and last date, unless

a minimum (second value) was reached. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Period is in hours. D is the estimated diameter (km). *diameter is from JPL Small Bodies Node. Other diameters

were derived from H and pV values. The last two columns give the a/b and b/c ratios based on the amplitude for an assumed triaxial ellipsoid viewed equatorially.

Number Name 2016 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Grp 1863 Antinous 08/06-08/10 159 42.6,40.2 7 0 7.471 0.005 0.33 0.02 NEA 468448 2003 LS3 07/05-07/08 146 23.7,23.2 299 16 5.325 0.005 0.32 0.02 NEA 468448 2003 LS3 08/23-08/25 148 8.5,8.3 327 4 5.329 0.005 0.02 0.02 NEA 469513 2003 QR79 09/02-09/04 95 11.4,15.3 335 7 4.11 0.01 0.18 0.03 NEA

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle values are for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

Number Name yyyy mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. U Exp 52381 1993 HA 2015 12/08-12/09 305 47.2,47.4 81 -30 4.107 0.002 0.58 0.01 3 120 138847 2000 VE62 2016 03/11-05/09 277 53.6,56.0 238 10 6.469 0.002 0.36 0.02 3 60

Table I. Observing circumstances and results. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). The U rating is our estimate and not necessarily the one assigned in the asteroid lightcurve database (Warner et al., 2009). Exp is average exposure, seconds. points. Keep the number of columns to a minimum and try to Standard Table for Observation Circumstances and Results avoid multi-line cells, except for headers. Any paper that reports on observations and results for lightcurve Tables should be numbered consecutively in Roman numerals, i.e. analysis needs to include a standardized table that contains a I, II, III, etc. The caption goes below the table. specific set of columns in specific order. This is to facilitate semi- automated data entry into large databases such as the asteroid Place tables at the end of the text, after any figures. The layout lightcurve database (LCDB; Warner et al., 2009). editor will place them how and where appropriate. Generally, use only white backgrounds for tables. Four examples of the standard table are shown above. These include the standard caption that goes below the table. The Please do not embed tables as objects, e.g., as an Excel spread paragraph uses the “Caption” paragraph style. As shown in some sheet table. It is permissible to use a Word table created in the of the examples, additional information can be included when document (Insert | Table), but not one that is an embedded object necessary. from another document. Other tables in the paper should not duplicate, if possible, the data Wide Tables in the standard table.

Do not use section breaks in order to span a table across the page. The standard table is not actually a MS Word table but text in a In fact, do not use section breaks of any kind anywhere in the text box that follows the guidelines mentioned above, i.e., for a 7” document. wide text box. Usually the text box will be at the top of a page, so it should be positioned at 0” from the top and left margins. In this If the table can fit into a single column, then you can place it in- case, the top wrapping would be 0” and the bottom wrapping line with the text. If the table needs to span both columns, create a would be 0.05-0.1”. If the table is at the bottom of a page, reverse text box and insert a Word table within the text box. the top/bottom wrapping numbers.

The text box should be 7” wide and use top/bottom word Keep in mind that your paper may not start at the top of an MPB wrapping. The internal margins of the box should be at 0.01-0.02” page, so the layout may change during final production. This is so that it’s possible to click on the text box rather than the why it is suggested that for tables with more than 2 or 3 lines be contents. placed towards the end of a paper. If the table is only 1-2 lines, it can be fit at the bottom of the first page or top of the second page, It is important to turn off the “Anchor to Text” (or “Move Object if there is one. with Text”) property of the text box in order to make it easier to change the layout of the paper as needed. Also, turn off “Allow The text in the table must use one of two paragraph styles: overlap” and “Layout in table cell.” LCHeader and LCData. The Word template (v2.2 and higher) includes these paragraph styles. These styles contain pre-set tabs Minor Planet Bulletin 44 (2017) 83 that account for the standard columns. For this reason, use tabs Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). and not spaces between the columns. “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258. The standard columns are, in order Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid 1. Number, blank entry if not numbered. Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sep. 2. Name or designation if not named. http://www.minorplanet.info/lightcurvedatabase.html 3. First and last dates in yyyy/mm/dd format. N.B. The “Updated” date for the LCDB changes periodically. Be 4. Number of data points used for analysis. sure to indicate the year/month for the version that you referenced. 5. Solar phase angle for the first and last date with a second, middle value if the phase angle reached a minimum during Figures the date range. Values are given to 0.1° precision and assumed to be for 0h UT on the give date. Do not use ± to Figures, if captioned, should be numbered consecutively in Arabic indicate after/before opposition. numerals. You can insert figures within the body of the text or at the end. 6. Phase angle bisector (PAB) longitude and latitude for the approximate mid-date of the observations at 0h UT. Use If your paper reports on one or more asteroids, each with an integer values. extended discussion and figure(s), we recommend embedding the 7. Rotation period, in hours figure(s) in line with the text. Such figures may or may not be captioned (see comments below about figure captions). 8. Error in rotation period, in hours. The precision should be the same as for the period. If your paper reports on many asteroids with only one short 9. Amplitude (peak-to-peak) of the lightcurve, in magnitudes paragraph and one or more figures for each, we recommend the to 0.01 mag precision, if appropriate. first paragraph of each asteroid begin with the number and 10. Error in amplitude, in magnitudes to 0.01 mag precision, if name/designation underlined and running on to the paragraph text. appropriate. The precision should be the same as for the You might insert the asteroid’s figure(s) after its text, or amplitude. alternately place all figures at the paper’s end. 11. “Flex” column. The default is a short entry to indicate the It is preferred that you insert the graphics yourself, even if only at group/family to which the asteroid belongs. If all the the end of the article, instead of supplying them as a set of files objects are the same group and this is mentioned in the that must be inserted by the editors. text, the entry can be blank (but still put a tab after the amplitude error value). The column can also be used to Please do not embed figures as objects, e.g., Excel charts. If show the exposure, filter, or other data. necessary, make a screen shot of the chart and edit it in a graphics editor. For example, in Windows, it is possible to highlight an If necessary, additional columns can be added to the end of the Excel chart in Excel, copy it, and paste it into the Paint program. line but not before the first column or between the standard columns. If values are not available, e.g., Points, enter a , If at all possible, use GIF or PNG format for all plots or charts to leaving the column blank. avoid “ringing” around small features that occurs when saving in JPG formation. BMP format files are much larger and can cause All data for each asteroid with the same observing circumstances problems when several megabytes in size. The JPG format should must fit on a single line (see the sample tables for an example of a be used if the figure is a gray-scale or color photo. table with two entries for the same asteroid). Use Insert | Picture | File on the Word main menu to insert If necessary, you can reduce the font size from the default of 8 graphics. If there are several consecutive figures, all but the last points, but do not go below 6.5 points, preferably 7 points. one should use the “Graphics” paragraph style. The last figure before any text, other than a caption, should use the “Normal” If necessary, the actual tab settings can be altered to help accommodate the data but, again, the order of the columns must be paragraph style. The picture wrapping style should be “In Line with Text.” correct, tabs must be used between columns, and the type of tab (left, right, decimal, centered) must be maintained. If inserting a figure that will span both columns, use a text box with appropriate wrapping to hold the figure. Do not use section To help with using the standard tables the first few times, copy/paste into your paper whichever of the four example tables breaks to change to a single column. It is very rare that a figure needs to be more than one column wide. above that most closely fits your needs and then substitute your data for those in the table. Figure captions should be used sparingly and offer new or expanded information. If, for example, a caption says only The data lines do not all have to use the same tab settings. As shown in one of the examples, one data line has only one date. The “Lightcurve for 1 Ceres phased to 9.078 h”, it is not needed since tab setting was modified for that line only to center it in the the standard table with circumstances and results (see above) will column. give the period and amplitude. You can also use text within the graphics to distinguish among them and reference the text in the Captions of the standard tables cite Harris et al. (1984) and body text instead of using a caption. Warner et al. (2009). Remember to include the corresponding references in your paper. For your convenience, the two references Use 300 dpi or higher resolution. Generally, use only white are reproduced immediately below and can be copied into your backgrounds for figures and solid colors for symbols. If the figure paper: is in color, make it such that the grayscale rendering of the figure Minor Planet Bulletin 44 (2017) 84 is easily legible. For example, yellow symbols on a white A space should separate a value and unit, e.g., 7.1334 h. An background are not suitable. Labeling should be large enough to exception to this is when the unit is used as part of a description, be easily readable when reproduced. e.g., 0.4-m telescope, 14-inch SCT, or 30-s exposures.

Avoid using color as the sole feature distinguishing data series in a If the unit falls onto the next line by itself, you can add a new line figure. The black-and-white rendering of the archival printed copy (Shift+Enter in Word) just before the first character of the value. of MPB might not show any differences. This will keep the value and unit together.

Lightcurve plot symbols should be easily differentiated from one If including a value and error, include the units only once, after the another. Each lightcurve should contain a legend that identifies error, e.g., 7.144 ± 0.005 h. each symbol with a date or other reference, the name of the object, the period (and error). If there is room, include the JD for zero “lightcurve” is a single word. phase or the first data point of a raw data plot, the period (and error) and amplitude (the error is not needed for the plot). Use a leading zero for a number whose absolute value is less than 1, e.g. 0.35 or –0.15. When adding a number of lightcurves at the end of a paper and to avoid a minimum of wasted white space, the original lightcurve When referring to a numbered asteroid that is named, do not put figures should have an aspect ratio of about 1.45: 1 (width:height) the number in parentheses, e.g., 1 Ceres instead of (1) Ceres. and use the Graphics paragraph style. This allows putting 8 plots on a single page (4 per column). When the asteroid is numbered but has only its MPC designation, put the number in parentheses, e.g., (178956) 2001 QN185. Note To make the lightcurves as readable as possible, the legend and that the number in the designation is not subscripted. Do not use other information should be moved to inside the plot area. A parentheses around the number if the number is a separate column tutorial on how this might be done is available at in a table. See “Standard Table for Observation Circumstances and Results” and the sample tables above. http://www.minorplanetobserver.com/MPOSoftware/ MPBPlots.htm Dates

See recent MPB issues for examples of how the above guidelines In order to standardize dates and avoid confusion due to different were applied. formats, we prefer that ANSI date format be used, i.e., year- month-day, e.g., 2010 Nov 12 or 2010 November 12. Equations and Special Symbols It is strongly recommended that all numeric dates not be used, e.g., If including equations with Greek characters or special symbols 2012-09-07, since it is not clear if the writer used the ANSI date for any reason, please use only Times New Roman, Arial, or format or not (see exception for tables below). Symbol (Windows TrueType) fonts. Use the extended characters of these fonts to insert special characters such as eastern European When using a month name and date, do not include a leading zero diacritical characters. This is done on a Windows machine by for a date from 1 to 9. For example, write Nov 7 instead of ALT+XXXX, where XXXX is a four-digit code entered on the Nov 07. numeric keypad. The Character Map system utility can also be used to locate and copy the necessary character. If using only the three-letter abbreviation for the month, it is not necessary to include the period after, i.e., instead of “Nov.” use If special characters are used, then – in addition to your “Nov”. manuscript – please submit a PDF that clearly shows how those characters should appear. If using only the month and year, put the year before the month, i.e., 2008 Nov or 2008 November.

In a table, such as giving a range of dates for observations, Accepted Abbreviations and Other Conventions numbers can be used to save space. The column head (or table caption) should clearly indicate the format, e.g., “mm/dd”. Unless The following abbreviations for units are preferred in the MPB: the year changes, include only the month and day in the table entries but indicate the year in the column header (or table arc minutes arcmin caption). arc seconds arcsec days d References degrees ° (Alt+0176, see notes under “Equations and Special Symbols”), or deg Authors should try to follow the standard reference styles for the hours h Minor Planet Bulletin. It can be tedious for an editor to fix out-of- magnitudes mag standard references. meters m minutes min References should be cited in the text such as Harris and Young pixel pix (1980) for one or two authors or Bowell et al. (1979) for more plus/minus ± (Alt+0177, see notes under “Equations and than two authors. If the author and year are within the parentheses, Special Symbols”) separate the author and year with a comma. If multiple references seconds s are given within parentheses, separate the references with a semicolon. For example: “The results are in good agreement with earlier works (Smith, 1999; Jones, 2010).”

Minor Planet Bulletin 44 (2017) 85

URLs (web addresses) should be italics, whether in the article Behred, R. (2002, 2005, 2006). Observatoire de Geneve web site. body or in a reference. If a URL is too long for one line, separate http://obswww.unige.ch/~behrend/page_cou.html after a slash or hyphen, or before a period. It is acceptable to start a URL on a line by itself, e.g. Please remove active hyperlinks from the document (usually indicated by the text being in blue or the default hyperlink text JPL (2016). Small Body Database Search Engine. color). These do not always convert to valid hyperlinks when http://ssd.jpl.nasa.gov/sbdb_query.cgi producing the final PDF document. The line preceding a URL can be left-justified by ending it with a The reference section should list papers in alphabetical order of tab, if needed, and newline (Shift+Enter in Word). the first author’s last name, then by year. Include the full list of authors in the citation in the References section, unless it exceeds Here are example entries for a journal article with page numbers, a 15. In that case, use “and xxx colleagues” (without the quotes) as journal article with article number, a chapter in a book, and a the “last author” where xxx is the number of unlisted authors. Use book. surname, initials for each author, separating author names with commas (e.g., Astronomer, J.Q., Assistant, H.I.S.). Bus, S.J., Binzel, R.P. (2002a). “Phase II of the Small Main-Belt Asteroid Spectroscopic Survey. The Observations.” Icarus 158, There are no blanks between initials. 106-145.

For references by multiple authors, omit the word “and” before the Jacobson, S.A., Scheeres, D.J., McMahon, J. (2014). “Formation final author, unless it is the “and xxx colleagues” case described of the Wide Asynchronous Binary Asteroid Population.” Ap. J. above. 780, A60.

Include the full title of the work in addition to the publication, Pravec, P., Harris, A.W., Michalowski, T. (2002). “Asteroid volume, and page numbers. Include both beginning and ending Rotations.” In Asteroids III (W.F. Bottke, A. Cellino, P. Paolicchi, page number for articles spanning more than one page. Many R.P. Binzel, eds.) pp 113-122. Univ. Arizona Press, Tucson. journals now give an article number instead of page range. In this Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry case, use AXX where XX is the article number. It is not necessary nd to include the number of pages after the article number. and Analysis (2 edition). pp 268. Springer, New York.

If several references are to the same web site and differ only in year, use a single reference with the several years instead of a separate reference for each year. For example,

IN THIS ISSUE Number Name EP Page Number Name EP Page 2083 Smither 12 12 4963 Kanroku 3 3 2100 Ra-Shalom 22 22 4963 Kanroku 66 66 This list gives those asteroids in this issue for 2108 Otto Schmidt 12 12 5143 Heracles 22 22 which physical observations (excluding 2136 Jugta 3 3 5349 Paulharris 67 67 astrometric only) were made. This includes 2150 Nyctimene 12 12 5427 Jensmartin 12 12 lightcurves, color index, and H-G 2189 Zaragoza 60 60 5587 1990 SB 22 22 determinations, etc. In some cases, no specific 2233 Kuznetsov 49 49 5836 1993 MF 22 22 results are reported due to a lack of or poor 2272 Montezuma 49 49 6138 1991 JH1 1 1 quality data. The page number is for the first 2284 San Juan 7 7 6382 1988 EL 12 12 2522 Triglav 3 3 6870 Pauldavies 12 12 page of the paper mentioning the asteroid. EP is 2581 Radegast 3 3 6911 Nancygreen 12 12 the “go to page” value in the electronic version. 2919 Dali 12 12 7341 1991 VK 22 22 3008 Nojiri 57 57 7350 1993 VA 52 52 Number Name EP Page 3042 Zelinsky 60 60 7588 1992 FJ1 3 3 153 Hilda 36 36 3105 Stumpff 69 69 7829 Jaroff 12 12 392 Wilhelmina 9 9 3232 Brest 60 60 7888 1993 UC 22 22 433 Eros 22 22 3352 McAuliffe 22 22 7959 Alysecherri 12 12 507 Laodica 3 3 3433 Fehrenbach 52 52 8360 1990 FD1 63 63 565 Marbachia 60 60 3443 Leetsungdao 12 12 8404 1995 AN 12 12 583 Klotilde 3 3 3493 Stepanov 7 7 8743 Keneke 36 36 637 Chrysothemis 12 12 3571 Milanstefanik 36 36 8783 Gopasyuk 49 49 699 Hela 12 12 3577 Putilin 36 36 10143 Kamogawa 3 3 775 Lumiere 69 69 3637 O'Meara 59 59 10150 1994 PN 52 52 864 Aase 9 9 3680 Sasha 1 1 10306 Pagnol 60 60 1027 Aesculapia 3 3 3733 Yoshitomo 3 3 10636 1998 QK56 22 22 1044 Teutonia 69 69 3743 Pauljaniczek 57 57 11152 Oomine 12 12 1084 Tamariwa 69 69 3792 Preston 52 52 11250 1972 AU 57 57 1090 Sumida 7 7 3843 OISCA 36 36 11386 1998 TA18 63 63 1095 Tulipa 69 69 3925 Tret'yakov 57 57 11542 Solikamsk 36 36 1154 Astronomia 1 1 3976 Lise 67 67 12676 1981 DU1 42 42 1212 Francette 36 36 4031 Mueller 12 12 14256 2000 AA96 42 42 1269 Rollandia 36 36 4132 Bartok 49 49 15278 Paquet 36 36 1293 Sonja 49 49 4132 Bartok 69 69 15350 Naganuma 67 67 1293 Sonja 60 60 4164 Shilov 12 12 16029 1999 DQ6 3 3 1293 Sonja 69 69 4317 Garibaldi 36 36 16585 1992 QR 49 49 1346 Gotha 60 60 4446 Carolyn 36 36 16681 1994 EV7 12 12 1715 Salli 11 11 4524 Barklajdetolli 67 67 16834 1997 WU22 22 22 1770 Schlesinger 52 52 4856 Seaborg 3 3 16843 1997 XX3 36 36 1863 Antinous 22 22 4923 Clarke 60 60 17428 Charleroi 36 36 1911 Schubart 3 3 4958 Wellnitz 3 3 19300 1996 SH6 49 49 Minor Planet Bulletin 44 (2017) 86

Number Name EP Page Number Name EP Page Number Name EP Page 19516 1998 QF80 57 57 71933 2000 WW61 42 42 375941 2009 WE102 42 42 19516 1998 QF80 60 60 72007 2000 XM7 12 12 376052 2010 EH44 42 42 20038 1992 UN5 36 36 73987 1998 EA2 42 42 385343 2002 LV 22 22 20163 1996 UG 42 42 80940 2000 DD86 42 42 425713 2011 BK24 20 20 20906 2727 P-L 42 42 87684 2000 SY2 22 22 452389 2002 NW16 22 22 22550 Jonsellon 42 42 91040 1998 FD14 42 42 458198 2010 RT11 52 52 23587 Abukumado 57 57 96842 1999 RH208 12 12 464797 2004 FZ1 22 22 23721 1998 HQ27 67 67 102912 1999 XA21 49 49 467336 2002 LT38 22 22 23974 1999 CK12 12 12 106538 2000 WK63 22 22 468448 2003 LS3 22 22 28992 2001 MW28 12 12 107924 2001 FO103 42 42 469513 2003 QR79 22 22 30019 2000 DD 49 49 110572 2001 TH115 42 42 469634 2004 SZ19 22 22 30251 Ashkin 42 42 117687 2005 EX259 42 42 470510 2008 CJ116 22 22 30958 1994 TV3 49 49 122092 2000 HZ50 42 42 471241 2011 BX18 22 22 32460 2000 SY92 36 36 125268 2001 VJ2 42 42 471241 2011 BX18 52 52 34742 2001 QD79 42 42 125979 2001 YU21 42 42 474163 1999 SO5 22 22 37801 1997 WO47 42 42 127288 2002 JV74 42 42 477162 2009 ES 22 22 40263 1999 FQ5 22 22 138847 2000 VE62 20 20 479325 2013 TV5 22 22 43003 1999 UC14 12 12 154244 2002 KL6 22 22 480004 2014 KD91 22 22 43692 2160 P-L 42 42 162117 1998 SD15 22 22 480004 2014 KD91 52 52 43956 Elidoro 42 42 163243 2002 FB3 20 20 1998 GL10 20 20 45209 1999 XT178 42 42 163348 2002 NN4 22 22 2005 TF 22 22 45898 2000 XQ49 12 12 163694 2003 DP13 49 49 2015 CA1 20 20 46818 1998 MZ24 49 49 211523 2003 QX60 42 42 2016 PN1 22 22 51874 2001 PZ28 36 36 221794 2008 BC34 42 42 2016 RB1 22 22 52381 1993 HA 20 20 228653 2002 EZ129 42 42 2015 SZ2 65 65 52750 1998 KK17 22 22 250458 2004 BO41 22 22 2016 HL 20 20 56591 2000 JP37 12 12 257838 2000 JQ66 22 22 2016 NA1 22 22 61652 2000 QO112 42 42 315098 2007 EX 20 20 2016 NH15 22 22 64787 2001 XH200 42 42 337069 1998 FX134 20 20 2016 NG33 22 22 66889 1999 VW78 42 42 347813 2002 NP1 22 22 2016 RP33 22 22 68278 2001 FC7 20 20 357024 1999 YR14 22 22 2016 LX48 22 22 68346 2001 KZ66 22 22 357024 1999 YR14 52 52 2016 LX48 52 52 70171 1999 OL2 3 3 370307 2002 RH52 22 22 2016 LX48 67 67 2016 CL264 22 22

THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly Authors should submit their manuscripts by electronic mail journal of the Minor Planets Section of the Association of Lunar and ([email protected]). Author instructions and a Microsoft Word template Planetary Observers (ALPO). Current and most recent issues of the MPB document are available at the web page given above. All materials must are available on line, free of charge from: arrive by the deadline for each issue. Visual photometry observations, http://www.minorplanet.info/mpbdownloads.html positional observations, any type of observation not covered above, and Nonmembers are invited to join ALPO by communicating with: Matthew general information requests should be sent to the Coordinator. L. Will, A.L.P.O. Membership Secretary, P.O. Box 13456, Springfield, IL 62791-3456 ([email protected]). The Minor Planets Section is * * * * * directed by its Coordinator, Prof. Frederick Pilcher, 4438 Organ Mesa Loop, Las Cruces, NM 88011 USA ([email protected], assisted by The deadline for the next issue (44-2) is January 15, 2017. The deadline Lawrence Garrett, 206 River Rd., Fairfax, VT 05454 USA for issue 44-3 is April 15, 2017. ([email protected]). Dr. Alan W. Harris (Space Science Institute; [email protected]), and Dr. Petr Pravec (Ondrejov Observatory; [email protected]) serve as Scientific Advisors. The Asteroid Photometry Coordinator is Brian D. Warner, Palmer Divide Observatory, 446 Sycamore Ave., Eaton, CO 80615 USA ([email protected]).

The Minor Planet Bulletin is edited by Professor Richard P. Binzel, MIT 54-410, 77 Massachusetts Ave, Cambridge, MA 02139 USA ([email protected]). Brian D. Warner (address above) is Associate Editor, and Dr. David Polishook, Department of Earth and Planetary Sciences, Weizmann Institute of Science ([email protected]) is Assistant Editor. The MPB is produced by Dr. Robert A. Werner, 3937 Blanche St., Pasadena, CA 91107 USA ([email protected]) and distributed by Derald D. Nye. Direct all subscriptions, contributions, address changes, etc. to:

Mr. Derald D. Nye - Minor Planet Bulletin 10385 East Observatory Drive Corona de Tucson, AZ 85641-2309 USA ([email protected]) (Telephone: 520-762-5504)

Effective with Volume 38, the Minor Planet Bulletin is a limited print journal, where print subscriptions are available only to libraries and major institutions for long-term archival purposes. In addition to the free electronic download of the MPB noted above, electronic retrieval of all Minor Planet Bulletin articles (back to Volume 1, Issue Number 1) is available through the Astrophysical Data System http://www.adsabs.harvard.edu/.

Minor Planet Bulletin 44 (2017)