The Minor Planet Bulletin 41 (2014) 158 Same Response

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

VOLUME 41, NUMBER 3, A.D. 2014 JULY-SEPTEMBER 139.

LIGHTCURVES FOR INVERSION MODEL CANDIDATES about asteroid discovery dates and names comes from the JPL small bodies database (JPLSBD, 2014). The list of observed Daniel A. Klinglesmith III, Jesse Hanowell, Ethan Risley, Janek asteroids is given Table 1. This table contains the asteroid number, Turk, Angelica Vargas, Curtis Alan Warren name, date range, solar phase angle, average solar bisector phase Etscorn Campus Observatory, New Mexico Tech angles, period determination, period error, amplitude, amplitude 101 East Road error. Table 2 summarizes the solar bisector phase angles of Socorro, NM USA 87801 published lightcurves for these asteroids. The previously observed [email protected] solar bisector phase angles were obtained from the Lightcurve data base (LCDB; Warner, 2014). (Received: 15 April) Individual Asteroids

We present lightcurves for 12 inversion model candidate 199 Byblis is a main-belt asteroid discovered by C.H.F. Peters at asteroids that will benefit from additional data at another Clinton on 1879 Jul 09. It is also known at 1971 WB. Behrend solar bisector phase angle. We obtained synodic periods reports four period results based on data from different observers: for each asteroid that were within ± 0.002 h. Most have F. Manzini (Behrend, 2008), P = 5.22024 h; R. Roy (Behrend shapes that differed from previously published 2006), P = 5.22024 h; R. Roy et al. (Behrend, 2005), P = 5.22012 lightcurves in both amplitude and shape. ± 0.000240 h; and S. Casulli and L. Bernasconi (Behrend, 2003), P = 5.22022 ± 0.0003. Hanus (2013) in the process of determining shape models reports a sidereal period of 5.22063 hours. We The observations of asteroid lightcurves were obtained at the observed 199 Byblis on 7 nights between 2014 Feb 18 and Apr 01. Etscorn Campus Observatory (ECO, 2014). We used three We can duplicate the periods of the previous researchers of 5.221 ± Celestron 0.35-m Schmidt-Cassegrain telescopes (SCTs) on 0.001 h with an amplitude of A = 0.08 ± 0.10 mag. However that Software Bisque Parmount ME mounts (SB, 2014). Two of the result has only one maximum and one minimum. If we double the telescopes used SBIG STL 1001E CCDs that have 1024x1024 24- period to 10.444 ± 0.001 with A = 0.09 ± 0.10 mag, we get a micron pixels. The third telescope used an SBIG ST10XME with bimodal lightcurve with a slightly better fit. an Optec 0.5x focal reducer. The ST10XME was binned 2x2 providing an image of 1092x736 13.6-micron pixels. The pixel 616 Elly is a main-belt asteroid discovered by A. Kopff at size for the STL-1001E cameras is 1.25 arcsec/pix. This provides a Heidelberg on 1906 Oct 17. It is also known as 1906 VT. Warner 22x22 arc minute field-of-view. The ST10 XME pixel size is 1.28 (2010) reports a period of 5.297 ± 0.003 h with A = 0.48 mag. arcsec/pix. This provides a 20x16 arc minute field-of-view. The Durkee (2010) reports a period of 4.30 ± 0.02 h with A = 0.38 mag. asteroid images were obtained through clear filters. Exposure times Mikulecka (2010) reports a period of 5.297 ± 0.001 h with A = varied between 2 and 5 minutes depending on the brightness of the 0.35 ± 0.05 mag. We observed 616 Elly on 8 nights between 2014 object. Each evening a series of 11 dome flats was obtained and Feb and Mar 22. Our period determination was 5.298 ± 0.002 h combined into a master flat with a median filter. The telescopes with A = 0.36 ± 0.05 mag. were controlled with Software Bisque’s TheSky6 (SB, 2014) and the CCDs were controlled with CCDsoft V5 (SB, 2014). The 620 Drakonia is a main-belt asteroid discovered by J. H. Metcaff at images were dark subtracted and flat field corrected using image Taunton on 1906 Oct 26. It is also known as 1906 WE, 1950 ET, processing tools within MPO Canopus version 10.4.1.9 (Warner, 1950 HS, and 1955 QE1. Warner (2002) reports a period of 5.485 2014). The multi-night data sets for each asteroid were combined ± 0.01 h with A = 0.52 ± 0.02 mag. Bin et al. (2011) report a with the FALC routine (Harris et. al., 1989) within MPO Canopus period of 5.480 ± 0.003 h with A = 0.08 ± 0.01 mag. We observed to provide synodic periods for each asteroid. 620 Drakonia for 9 nights between 2014 Feb 09 and Mar 24. Our period determination is 5.487 ± 0.001 h with A = 0.65 ± Observed Asteroids 0.05 mag.

The 12 asteroids observed were taken from the list of possible 822 Lalage is a main-belt asteroid discovered by M. Wolf at inversion model candidates by Warner et al. (2014). All have Heidelberg on 1916 Mar 31. It is also known as 1916 ZD and 1943 periods less than 8 hours. This allowed us, in many cases, to obtain EJ1. Wisniewski et al. (1995) reported a period of 3.345 ± 0.001 h. at least one complete cycle per observing night. The information Higgins (2011) reported a period of 3.3465 ± 0.0006 h with A = Minor Planet Bulletin 41 (2014) Available on line http://www.minorplanet.info/mpbdownloads.html 140

Table 1. Current results

# Name 2014 (mm/dd) UT Phase PABL PABB Period P. E Amp A.E. 199 Byblis 02/18 - 04/01 13.6,7.4, 7.6 185 18 5.221 0.001 0.1 0.07 616 Elly 02/18 - 03/22 4.6,4.1,13.4 153 7 5.298 0.002 0.4 0.05 620 Drakonia 02/09 - 03/24 7.8,4.1,14.1 115 8 5.487 0.001 0.7 0.05 822 Lalage 02/08 - 03/11 1.7, ,16.1 143 -1 3.346 0.001 0.5 0.10 855 Newcombia 03/25 - 04/07 8.3, , 0.8 198 0 3.003 0.001 0.3 0.05 1044 Teutonia 01/27 - 02/21 4.4, ,13.1 116 4 3.157 0.001 0.3 0.10 1219 Britta 02/12 - 03/17 19.9, ,27.3 113 5 5.575 0.001 0.7 0.10 1294 Antwerpia 03/19 - 03/24 12.8, ,14.2 146 10 6.623 0.001 0.4 0.10 1299 Mertona 04/02 - 04/04 18.2, ,18.7 144 -2 4.978 0.002 0.6 0.10 1321 Majuba 03/13 - 03/29 2.4, , 6.7 170 -6 5.221 0.001 0.4 0.10 2381 Landi 01/21 - 03/25 5.7, ,23.4 118 -8 3.986 0.001 0.9 0.05 3573 Holmberg 01/27 - 03/25 9.0, ,27.4 115 -2 6.543 0.001 0.9 0.10

Table 2. Previous Solar Bisector Phase Angles

number name reference Date PABL PABB 199 Byblis Behrend 2003web 2003 Apr 08 218.5 25.9 199 Byblis Behrend 2005web 2005 Nov 09 46.5 -12 199 Byblis Behrend 2006web 2006 Dec 20 100.8 3.2 199 Byblis Behrend 2008web 2008 Feb 09 159.3 17

616 Elly Warner 2010 MPB 37, 112 2010 Jan 31 161.8 7.2 616 Elly Durkee 2010 MPB 37, 125 2010 Feb 24 162.6 5.4 616 Elly Mikulecka 2011web 2010 Mar 03 162.6 4.9

620 Drakonia Warner 2002b MPB 29, 27 2001 Nov 05 42.9 7.3 620 Drakonia warner 2011f MPB 38, 52 2001 Nov 05 42.9 7.3 620 Drakonia Bin 2011 MPB 38, 179 2001 Mar 02 190.2 -0.7

822 Lalage Wisniewski 1992 Sep 25 0.1 0.5 822 Lalage Higgins 2011a MPB 38,41 2009 Oct 09 9.8 0.3 822 Lalage Stephens 2014 web 2014 Jan 14 139.2 -1

855 Newcombia Cooney 2007 MPB 34, 47 2004 Oct 14 9 -1.4

1044 Teutonia Behrend 2006 web 2006 Jan 11 139.1 5 1044 Teutonia Betzler 2008b MPB 35, 26 2007 Jun 08 256.3 -1.7 1044 Teutonia Behrend 2012 web 2012 Nov 13 28.8 -2.4

1219 Britta Behrend 2003 web 2003 Dec 26 79.4 4.4

1294 Antwerpia Lecrone 2005 MPB 32, 46 2005 Feb 02 127.7 8.4 1294 Antwerpia Behrend 2005web 2006 Mar 26 206.1 9 1294 Antwerpia Stephens 2014web 2014 Jan 16 146.3 9.2

1299 Mertona Monson 2004 MPB 31, 97 2003 Nov 25 50.2 -9.9 1299 Mertona Behrend 2005web 2005 Mar 14 179 2.1

1321 Majuba Ditteon 2007 MPB 34, 59 2006 Nov 09 42.1 11.8 1321 Majuba Behrend 2006web 2006 Nov 11 42.1 11.8

2381 Landi

3573 Holmberg Galad 2008 MPB 35, 78 2007 Jan 12 63.6 0.8

0.58 ± 0.01 mag. We observed 822 Lalage for 6 nights between for 9 nights between 2014 Mar 25 and Apr 07. Our period 2014 Feb 08 and Mar 11. Our period determination was 3.346 ± determination agrees with Cooney et al.: 3.003 ± 0.001 h with A = 0.001 h with A = 0.53 ± 0.10 mag. 0.33 ± 0.05 mag and a very similar shape.

855 Newcombia is a main-belt asteroid discovered by S. 1044 Teutonia is a main-belt asteroid discovered by K. Reinmuth Belyavskij at Simeis on 1916 Apr 03. It is also known as 1935 SJ1 at Heidelberg on 1924 May 10. It is also known as 1924 RO, 1925 and 1938 KB. Cooney et al. (2007) reported a period of 3.003 ± XF, 1929 RP, 1949 KX, 1954 UY1, 1958 RG, 1958 UP, and A907 0.007 h with A = 0.35 ± 0.03 mag. We observed 855 Newcombia EE. Behrend reports two provisional period results: P. Antonini Minor Planet Bulletin 41 (2014) 141

(Behrend, 2006), P = 3.1848 ± 0.024 h, and R. Roy (Behrend, References 2012), P = 3.15336 ± 0.00026 h. Betzler et al. (2008) published a period of 2.84 ± 0.04 h with A = 0.20 ± 0.03 mag. We observed Almeida, R., Angeli, C.A., Duffard, R., Lazzaro, D., (2004). 1044 Teutonia for 6 nights between 2014 Jan 27 and Feb 21. Our “Rotation periods for small main-belt asteroids.” A&A 415, 403- period determination was 3.157 ± 0.001 h with A = 0.29 ± 0.10 406 mag. Behrend,R. (2003, 2005, 2006, 2008, 2012). 1219 Britta is a main-belt asteroid discovered by M. Wolf at http://obswww.unige.ch/~behrend/page_cou.html Heidelberg on 1932 Feb 06. It is also known as 1932 CJ. Pilcher et al. (1985) reported a period of 5.575 ± 0.001 h with A = 0.5 mag. Betzler, A.S., Ferreira, D.H., Ribeiro dos Santos, T.H., Novaes, Binzel et al. (1987) reported in improved period of 5.57497 ± A.B. (2008). “Lightcurve and Rotation Period of 1044 Teutonia.” 0.00013 h with the amplitude ranging between 0.60 and 0.70 mag. Minor Planet Bul. 35, 26 Behrend (2003) reports a period from L. Bernascone of 5.35752 ± 0.003 h. We observed 1219 Britta for 4 nights between 2014 Feb Bin, L., Haibin, Z., Jingshen, Y. (2011). “The Lightcurve Analysis 12 and Mar 17. Our period determination was 5.575 ± 0.001 h with of Five Asteroids.” Minor Planet Bul. 38, 179-180. A = 0.69 ± 0.10 mag. Binzel, R.P., Cochran, A.L., Barker, E.S., Tholen, D.J., Barucci, 1294 Antwerpia is a main-belt asteroid discovered by E. Delporte A., di Martino, M., Greenberg, R., Weidenschilling, S.J., at Uccle on 1933 Oct 24. It is also known as 1933 UB1, 1930 AF, Chapman, C.R., Davis, D.R. (1987). “Coordinated observations of 1932 LC, 1964 XF, and A917 DB. Almeida et al. (2004) reported a asteroids 1219 Britta and 1972 Yi Xing.”, Icarus 71, 148-158. period of 6.63 h. LeCrone et al. (2005) reported a period of 6.63 ± Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.” 0.001 h with A = 0.40 mag. Behrend (2006) reported a period from Icarus 72, 135-208. L. Bernasconi of 6.622496 ± 0.00001 h. We observed 1294 on 5 nights between 2014 March 19 and March 24.We obtained a Cooney, W.R., Gross, J., Terrell, D., Reddy, V., Dyvig, R. (2007). period of 6.623 ± 0.001 h with A = 0.35 ± 0.10 mag. “Lightcurve results for 486 Cremona, 855 Newcombia, 942 Romilda, 3908 Nyx, 5139 Rumoi, 5653 Camarillo, (102866) 1999 1299 Mertona is a main-belt asteroid discovered by G. Reiss at WA5.” Minor Planet Bul. 34, 47-49. Algiers on 1934 Jan 18. It is also known as 1934 BA. Monson and Kipp (2004) reported a period of 4.977 ± 0.003 h with A = 0.55 Ditteon, R., Hawkins, S. (2007). “Asteroid Lightcurve Analysis at mag. Behrend (2005) reported a period 4.98072 ± 0.002 h from Oakley Observatory - November 2007.” Minor Planet Bul. 34, 59- work by R. Roy. We observed 1299 Majuba for 3 nights between 63. 2014 Mar 02 and Mar 04. We obtained a period of 4.978 ± 0.002 h with A = 0.59 ± 0.10 mag. Durkee, R.I. (2010). “Asteroids Observed from The Shed of Science Observatory 2009 October - 2010 March.” Minor Planet 1321 Majuba is a main-belt asteroid discovered by C. Jackson at Bul. 37, 125-127. Johannesburg on 1934 May 07. It is also known as 1934 JH, 1928 FH, 1930 UW, 1935 SG, 1950 QE, 1950 QQ, 1950 RE, 1950 RK1, ECO (2014). Etscorn Campus Observatory 1950 RQ, 1964 GD, and A908 FD. Binzel (1987) reported that his http://www.mro.nmt.edu/education-outreach/etscorn-campus- data were consistent with either 6.78 h or 5.4 h. Ditteon and observatory Hawkins (2007) confirmed a period of 5.207 ± 0.009 h with A = 0.25 ± 0.05 mag. We observed 1321 Majuba on 5 nights Galad, A., Kornos, L. (2008). “A sample of Lightcurves from between 2014 Mar 13 and Mar 29. We obtained a period of 5.221 Modra.” Minor Planet Bul. 35, 78-81. ± 0.001 h with A = 0.35 ± 0.10 mag. Harris, A.W., Young, J.W., Bowell, E., Martin, L. J., Millis, R.L., 2381 Landi is a main-belt asteroid discovered by F. Aguilar at El Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Leoncito on 1976 Jan 03. It is also known at 1976 AF. Almeida et H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, al. (2004) reported a period of 3.91 h. We observed 2391 Landi for 24, 60, 261, and 863.” Icarus 77, 171-186. 5 nights between 2014 Jan 18 and Mar 25. We obtained a period of 3.986 ± 0.001 h with A = 0.88 ± 0.05 mag. JPLSBD, Small Body Database Search Engine. http://ssd.jpl.nasa.gov/sbdb_query.cgi 3573 Holmberg is a main-belt asteroid discovered by K. Olofsson at La Silla on 1982 Aug 16. It is also known at 1982 QO1, 1929 LeCrone, C., Addleman D., Butler, T., Hudson, E., Mulvhill, A., WN, 1947 BL, 1976 YW1, and 1979 WH5. Galad and Kornos Reichert, C., Ross, I., Ditteon, R. (2005). “2004-2005 Winter (2008) reported a synodic period of 6.5431 ± 0.0001 h with A = Observing Campaign at Rose-Hulman Institute: Results for 1098 1.03. We observed 3573 Holmberg on 5 nights between 2014 Jan Hakone, 1182 Ilona, 1294 Antwerpia, 1450 Raimonda, 2251 27 and Mar 25. We obtained a period of 6.543 ± 0.001 h with A = Tihkov, and 2365 Interkosmos.” Minor Planet Bul. 32, 46-48. 0.91 ± 0.1 mag. Mikulecka, B. (2011). Entry on CALL web site. Acknowledgments http://www.minorplanet.info/call.html

The Etscorn Campus Observatory operations are supported by the Monson, A., Kipp, S. (2004). “Rotational periods of Asteroids Research and Economic Development Office of New Mexico 1165 Imprinetta, 1299 Mertona, 1645 Waterfield, 1833 Shmakova, Institute of Mining and Technology (NMIMT). Student support at 2313 Aruna and (13856) 1999 XZ105.” Minor Planet Bul. 31, 71- NMIMT is given by NASA EPSCoR grant NNX11AQ35A, the 73. Department of Physics, and the Title IV of the Higher Education Act from the Department of Education.

Minor Planet Bulletin 41 (2014) 142

Pilcher, F., Binzel, R.P., Tholen, D.J. (1985). “Rotations of 1168 Brandia and 1219 Britta.” Minor Planet Bul. 12, 10.

Software Bisque (SB) (2014). http://www.bisque.com/sc/

Warner, B.D. (2002). “Asteroid Photometry at the Palmer Divide Observatory: Results for 620 Drakonia, 3447 Burkhalter, and 7816 Hanoi.” Minor Planet Bul. 29, 27-28.

Warner. B.D. (2014). MPO Canopus software. http://www.minorplanetobserver.com/MPOSoftware/ MPOCanopus.htm

Warner, B.W, Harris, A.W., Pravec, P. (2014). LCDB update: http://www.minorplanet.info/lightcurvedatabase.html

Warner, B.D., Harris, A.W., Pravec, P., Durech, J., Benner, L.A.M. (2014). “Lightcurve Photometry Opportunities: 2014 January-March.” 40, 61-65.

Wisniewski, W.Z., Michalowski, T.M., Harris, A.W., McMillan, R.S. (1995). “Photoelectric Observations of 125 Asteroids.” Abstracts of Lunar and Planetary Science Conference. 26, 1511.

Minor Planet Bulletin 41 (2014) 143

CORRIGENDUM

Fauvaud, S., and Fauvaud, M. (2013). “Photometry of minor planets. I. Rotation periods from lightcurve analysis for seven main-belt asteroids.” Minor Planet Bulletin 40, 224-229.

In the Data Reduction Section, a term has been forgotten during the writing process of the weighted differential magnitude (Δm) of the asteroid. The right Eq. (3) is the following one:

Minor Planet Bulletin 41 (2014) 144

ASTEROID LIGHTCURVE ANALYSIS AT In the plots below, the “Reduced Magnitude” is Johnson V (or CS3-PALMER DIVIDE STATION: Cousins R) as indicated in the Y-axis title. These are values that 2014 JANUARY-MARCH have been converted from sky magnitudes to unity distance by applying –5*log (rΔ) to the measured sky magnitudes with r and Δ Brian D. Warner being, respectively, the Sun-asteroid and Earth-asteroid distances Center for Solar System Studies / MoreData! in AU. The magnitudes were normalized to the phase angle given 446 Sycamore Ave. in parentheses, e.g., alpha(6.5°), using G = 0.15, unless otherwise Eaton, CO 80615 USA stated. The horizontal axis is the rotational phase, ranging from [email protected] –0.05 to 1.05.

(Received: 28 March) For the sake of brevity, only some of the previously reported results may be referenced in the discussions on specific asteroids. For a more complete listing, the reader is directed to the asteroid Lightcurves for 40 main-belt asteroids were obtained at lightcurve database (LCDB; Warner et al., 2009a). The on-line the Center for Solar System Studies-Palmer Divide version at http://www.minorplanet.info/lightcurvedatabase.html Station (CS3-PDS) from 2014 January through March. allows direct queries that can be filtered a number of ways and the The majority of the objects were members of the results saved to a text file. A set of text files of the main LCDB Hungaria group/family. In many cases, the observations tables, including the references with bibcodes, is also available for were follow-up to previous apparitions to check for the download. Readers are strongly encouraged to obtain, when possibility of undiscovered satellites or to provide possible, the original references listed in the LCDB for their work. additional data for spin axis and shape modeling. One Hungaria, 5175 Ables, showed indications of a satellite Individual Results in the form of having two periods. However, there were no decisive observations of mutual events due to a 110 Lydia. The rotation period for this outer main-belt asteroid had satellite. This makes the asteroid a possible, but not been reported several times before the CS3-PDS observations in probable, binary. 2014 January: Pray (2004, 10.924), Warner et al. (2009f, 10.925808), and Stephens and Warner (2013, 10.928), among others. The most recent observations were in support of radar work CCD photometric observations of 40 asteroids were made at the by Shepard (see Shepard et al., 2010). The results from the 2014 Center for Solar System Studies-Palmer Divide Station (CS3-PDS) data analysis show an interestingly shaped lightcurve with a in 2014 January through March. Table I gives a listing of the synodic period that agrees with the earlier results. telescope/CCD camera combinations used for the observations. All the cameras use CCD chips from the KAF blue-enhanced family 323 Brucia. Brucia is a Mars-crosser, meaning its orbit takes it and so have essentially the same response. The pixel scales for the between Earth and Mars but not close enough to Earth’s orbit to be combinations range from 1.24-1.60 arcsec/pixel. considered a near-Earth asteroid (NEA). The CDS-PDS results were P = 9.463 ± 0.005 h and A = 0.26 ± 0.02 mag. The period Desig Telescope Camera PDS-1-12N 0.30-m f/6.3 Schmidt-Cass ML-1001E agrees with previous results from Schober et al. (1993. 9.46 h) and PDS-1-14S 0.35-m f/9.1 Schmidt-Cass FLI-1001E Behrend (2006, 9.4602 h). PDS-2-14N 0.35-m f/9.1 Schmidt-Cass STL-1001E PDS-2-14S 0.35-m f/9.1 Schmidt-Cass STL-1001E 428 Monachia. A member of the Flora group, this asteroid was PDS-20 0.50-m f/8.1 Ritchey-Chretien FLI-1001E chosen as a full moon project, meaning it could be worked near the Table I. List of CS3-PDS telescope/CCD camera combinations. time of full moon when the main targets of the CS3-PDS program, NEAs and Hungarias, could not. Wisniewski et al. (1997) reported All lightcurve observations were unfiltered since a clear filter can a period of 3.63384 h, Behrend (2007) found 3.6335 h, and result in a 0.1-0.3 magnitude loss. The exposure duration varied Kryszczynska et al. (2012) reported 3.6342 h. depending on the asteroid’s brightness and sky motion. Guiding on a field star sometimes resulted in a trailed image for the asteroid. 434 Hungaria. This is the third apparition at which the author observed the largest member and namesake of the Hungaria family Measurements were done using MPO Canopus. If necessary, an (Warner, 2010a; 2011f). The period found from the data obtained elliptical aperture with the long axis parallel to the asteroid’s path in 2014 February and March was 26.521 ± 0.001 h and in was used. The Comp Star Selector utility in MPO Canopus finds agreement with the earlier results. G = 0.43 was used in the up to five comparison stars of near solar-color to be used in analysis (Warner et al., 2009a). differential photometry. Catalog magnitudes are usually taken from the MPOSC3 catalog, which is based on the 2MASS catalog 495 Eulalia. Analysis of the data obtained at CS3-PDS in 2014 (http://www.ipac.caltech.edu/2mass) but with magnitudes March for this Nysa member gave P = 28.829 ± 0.006 h and converted from J-K to BVRI using formulae developed by Warner A = 0.11 ± 0.01 mag. The period differs slightly from the previous (2007). When possible, magnitudes are taken from the APASS result by the author of 28.967 h (Warner, 2013b). This could be catalog (Henden et al., 2009) since these are derived directly from due in part to the small gap in coverage in the latest lightcurve. reductions based on Landolt standard fields. Using either catalog, the nightly zero points have been found to be consistent to about 852 Wladilena. This Phocaea member was another full moon ± 0.05 mag or better, but on occasion are as large as 0.1 mag. This project. Harris et al. (1999) found a period of 4.6134 h and consistency is critical to analysis of long period and/or tumbling Behrend (2010) reported 4.6133 h. The result of this work was asteroids. Period analysis is also done using MPO Canopus, which 4.610 ± 0.002 h. implements the FALC algorithm developed by Harris (Harris et al., 1989). 1019 Strackea. This was the third apparition for this Hungaria to be worked by the author (Warner, 2009e, 4.044 h; 2011f, 4.047 h).

Minor Planet Bulletin 41 (2014) 145

2014 Number Name mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 110 Lydia 01/10-01/13 1024 10.0,9.0 135 7 10.927 0.005 0.14 0.01 323 Brucia 01/19-01/23 369 19.3,18.8 176 26 9.463 0.005 0.26 0.02 428 Monachia 03/17-03/19 119 21.9,22.2 127 6 3.633 0.002 0.34 0.02 434 Hungaria 02/24-03/22 1084 25.2,16.8 202 10 26.521 0.001 0.75 0.02 495 Eulalia 03/08-03/25 1439 10.1,3.1 191 0 28.829 0.006 0.11 0.01 852 Wladilena 02/14-02/15 239 19.5,19.3 196 10 4.61 0.002 0.25 0.02 1019 Strackea 01/15-01/17 185 27.3,26.9 167 6 4.052 0.002 0.24 0.02 1025 Riema 02/09-02/11 138 15.2,14.0 162 -6 3.591 0.003 0.12 0.01 1360 Tarka 01/16-02/04 216 16.9,18.0 58 24 8.858 0.001 0.43 0.02 1600 Vyssotsky 01/16-01/18 147 31.8,31.6 170 27 3.205 0.003 0.15 0.02 1626 Sadeya 02/13-02/15 239 32.4,32.6 86 -2 3.42 0.001 0.15 0.01 1656 Suomi 03/19-03/19 185 16.1,16.1 159 -7 2.59 0.01 0.13 0.01 3101 Goldberger 02/04-02/11 143 15.1,11.2 161 -1 5.268 0.001 0.9 0.03 3266 Bernardus 01/13-01/15 273 23.2,22.7 153 19 10.757 0.005 1.14 0.02 3309 Brorfelde 01/14-01/20 424 29.3,28.2 161 25 2.503 0.001 0.10 0.01 3800 Karayusuf 03/16-03/17 97 32.1,31.8 200 27 2.221 0.005 0.19 0.02 4440 Tchantches 01/14-01/17 119 30.3,30.7 55 15 2.788 0.001 0.22 0.02 4464 Vulcano 01/10-01/13 223 22.6,13.4 128 24 3.203 0.001 0.22 0.02 4490 Bambery 01/13-01/15 212 24.3,23.6 155 6 5.822 0.001 1.07 0.02 5175 Ables 01/16-01/26 358 26.4,28.3 67 -9 2.7976* 0.0005 0.06 0.01 5253 1985 XB 03/19-03/20 123 32.5,32.2 214 34 3.053 0.005 0.21 0.02 5871 Bobbell 01/14-01/23 233 31.0,32.0 66 23 28.90 0.03 0.31 0.03 6107 Osterbrock 01/19-01/23 193 22.8,24.3 84 -11 2.215 0.002 0.06 0.01 6493 Cathybennett 02/09-02/12 189 21.8,20.9 179 15 3.48 0.002 0.23 0.02 6517 Buzzi 02/04-02/21 145 14.8,22.4 112 -3 8.642 0.002 0.84 0.03 9165 Raup 02/12-03/07 673 16.1,10.2 165 19 560 25 1.05 0.1 13578 1993 MK 01/16-01/19 99 24.2,23.6 163 20 3.955 0.002 0.55 0.03 15374 Teta 02/12-02/14 98 8.5,8.3 151 14 2.82 0.005 0.3 0.03 15964 Billgray 01/16-01/17 157 28.2,28.4 74 17 3.565 0.003 0.21 0.02 16562 1992 AV1 01/23-02/04 300 26.5,23.8 166 24 20.18 0.05 0.23 0.02 17590 1995 CG 02/06-02/26 371 12.0,20.6 119 -6 49.6 0.3 0.4 0.05 ”” ”” 2012 06/23-07/13 202 21.0,23.3 266 27 47.4 0.2 0.55 0.10 21688 1999 RK37 02/24-02/25 156 5.704 0.005 0.68 0.03 44600 1999 RU10 03/05-03/09 90 30.1,30.8 112 12 6.206 0.005 1.09 0.03 48601 1995 BL 01/03-01/05 124 20.9,19.9 133 3 4.60 0.01 0.50 0.02 49667 1999 OM2 03/05-03/09 83 28.6,29.3 111 -9 3.49 0.002 0.6 0.03 53530 2000 AV200 01/05-01/06 108 19.7,19.2 136 4 4.310 0.005 0.34 0.02 69142 2003 FL115 03/05-03/09 107 19.8,21.3 138 -14 7.368 0.005 0.53 0.03 69406 1995 SX48 03/05-03/08 79 25.0,26.1 126 -11 4.487 0.005 0.19 0.02 86217 1999 TB35 03/12-03/14 211 29.7,30.0 129 23 5.994 0.003 0.88 0.03 118337 1999 BQ9 03/15-03/15 142 27.2,27.2 164 33 2.858 0.007 0.36 0.02 Table II. Observing circumstances. * Solution is for a primary of a binary asteroid (see text). 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, unless two values are given (first/last date in range).

1025 Riema. The lightcurve amplitude for this Hungaria is usually 3.205 h. Despite the extensive data set covering a number of years, on the order of 0.10 mag., making it a challenge to find a definitive attempts to find a definitive spin axis for Vyssotsky have not been period. It was observed at CS3-PDS in 2014 January for two successful, not even to where it can be said with certainty that the nights, each run covering more than a full cycle of the presumed asteroid is in prograde or retrograde rotation. period of about 3.6 h. Analysis found P = 3.588 h. Previous results include Warner (2009e, 3.566 h; 2013a, 3.581 h) and Stephens 1626 Sadeya. Sadeya is a Phocaea member and was another full (2003), who reported 3.580 h. The data set from 2009 was sparser moon project. A period of 3.420 h was found from the 2014 than the others and had greater scatter, which may explain why the February observations. This is in keeping with previous results by 2009 result is several sigmas removed from the others. Florczak et al. (1997, 3.438), Behrend (2009, 3.42048), Oey and Krajewski (2008, 3.4200), and Warner (2010e, 3.414). 1360 Tarka. Tarka is a middle main-belt object. It was a target of opportunity, meaning it was in the same field as a program target 1656 Suomi. Stephens (2004), Brinsfield (2008), and Warner for one or more nights. The only previously reported result was by (2009d, 2012) all found a period of about 2.59 h for this Hungaria the author (Warner, 2005b; 8.87 h). This is in good agreement with member, as did the analysis of the 2014 observations. Suomi was the period of 8.858 h found for this work. observed only one night (2014 March 19) since its period was already well-known and the run covered more than two rotations. 1600 Vyssotsky. Vyssotsky is the space occupied by the Hungarias The main goal was to get the basic shape of the lightcurve at the but, given its taxonomic classification of A, it is likely an 2014 apparition for future modeling. interloper and not a member of the Hungaria family, which are type E. It has been observed several times before: Higgins (2008), 3101 Goldberger. The only previous result for this Hungaria Warner (1999, 2009d, 2011b), and Warner et al. (2006a). All member was by Wisniewski et al. (1997), who reported P = 5.2 h results were in very close agreement with the 2014 period of Minor Planet Bulletin 41 (2014) 146 and amplitude of 0.96 mag. The 2014 parameters were 5.268 h and Warner (2009e, 5.823 h; 2011f, 5.816 h; and 2012, 0.90 mag. 5.827 h).

3266 Bernardus. This was the fourth apparition for this Hungaria 5175 Ables. When observed in 2010 (Warner, 2011a) and 2013 member to be worked by the author (see Warner, 2009e, 2011f, (Warner, 2014), there were no indications of a satellite. When the and 2012). All were in close agreement with the period of Hungaria member was re-observed in 2014 January, there 10.757 h found from the 2014 February observations. appeared to be a second period involved. The “P1: No Sub” plot shows the lightcurve assuming a single period. The “P1” and “P2” 3309 Brorfelde. This is a known binary, discovered by Warner et plots show lightcurves with periods of 2.7976 h and 10.44 h, al. (2005c; 2011c). The primary period (“P1” plot) in all cases was respectively. There were no obvious mutual events due to a very close to 2.500 h while the orbital period of the satellite (“P2”) satellite. The second period could be due to the rotation of a of about 18.5 hours was revealed by mutual events (occultations second, unconfirmed, satellite. This asteroid should be observed and/or eclipses involving the satellite). The events barely rose carefully (high precision photometry) at future apparitions. above the noise during the 2014 apparition. In fact, the “P1: No sub” plot shows that if the asteroid had not been known to be a (5253) 1985 XB. Skiff (2011) reported a period of 2.95 h based on binary, the deviations in the uncorrected lightcurve might have an observing run of five hours on a single night. Even with the data been written off as excessive noise. covering more than one rotation, there can still be a noticeable error in the period without data from a second, preferably 3800 Karayusuf. Observations by Warner (2008c) appeared to consecutive, night. The 2014 CS3-PDS data set covered two show evidence of a mutual event due to a satellite on one night. consecutive nights with each observing run covering more than However, there were no confirming observations. Because of this, one rotation. The analysis result was P = 3.053 h. the asteroid has been a priority at each apparition to see if conclusive evidence could be found. The 2014 data showed 5871 Bobbell. This Hungaria was observed in 2014 January to nothing suspicious. This would be expected since the viewing follow up on a period of 30.21 h reported by Warner (2009b). aspect based on the phase angle bisector was nearly identical for Unfortunately, the 2014 campaign data set was of lesser quality, the two apparitions, just as it was for the 2010 apparition (Warner, which likely lead to a period (P = 29.3 h) that was not in better 2010b). Regardless, the periods found over the years for the agreement with the earlier result. “primary” (or sole) body are in close agreement. 6107 Osterbrock. Despite an amplitude of 0.09 mag, the period of 4440 Tchantches. Past results include Warner et al. (2006b, 2.372 h derived from observations in 2012 (Warner, 2012) seemed 2.7883 h), Warner and Higgins (2009c, 2.7883 h), and Warner secure, especially when the period spectrum showed a sharp (2011a, 2.790 h; 2014, 2.7886 h). A re-examination of data minimum at 2.372 hours and no ambiguities. The same could not obtained in 2005 (Warner, 2014) showed signs of the asteroid be said for the analysis of the 2014 January data set. The period being binary. No indications were found in the observations from spectrum was mostly flat and showed a preference for a period >8 2013 October (Warner, 2014) or in the most recent data set. hours. The plot shows the result when limiting the period search from 2.000 to 3.000 hours, i.e., P = 2.215 h or about 0.12 hours 4464 Vulcano. Observations of this Hungaria at CS3-PDS in 2014 shorter. This result is not considered reliable and so the one from January revealed well-defined bimodal lightcurve with a period of 2012 should stand. 3.203 h and 0.22 mag amplitude. The period agreed with the result obtained in 2010 (Warner et al., 2011g) but not the one from 2007 6493 Cathybennett. The periods from the 2014 campaign and from (Warner, 2008a) when a period of 6.419 h was reported. The 2009 (Warner, 2009e) and 2011 (Warner, 2011f) are in good amplitude in 2007 was only 0.12 mag, which could mean that the agreement. double period was found. Looking at the period spectrum from that year, the RMS fit minimums at 3.2 and 6.4 h are essentially 6517 Buzzi. Results from previous campaigns (Warner 2005a, identical. 2009d, and 2012) and the one in 2014 are in agreement.

One way to resolve the ambiguity is to use what is called a “split 9165 Raup. Given its estimated size (5 km) and period of 560 halves plot” as outlined by Harris et al. (2014). Here, the full hours, this Hungaria “ought to be tumbling” (see Pravec et al., period (P) is used but the data are plotted using the half-period 2014, and references therein). There are slight indications of this in (P/2). This results in the second half of the lightcurve overlaying that the slopes of some of the sessions doesn’t quite match the the first half. In the split haves plot using the 2007 data set at 6.4 slope of the Fourier model curve. However, without coverage into hours, open black (dark) circles represent data from 0.0 to 0.5 a second rotation, where tumbling would show itself by the data rotation phase of the full period. Red (lighter) stars represent data not all fitting a single period, the evidence is too little to make any from 0.5 to 1.0 rotation phase. The two halves are essentially certain claims. identical, meaning that there is a possibility that the half-period is the correct solution. If the two halves had diverged significantly, (13578) 1993 MK. Initial results by Warner (e.g., 2008b) gave a the half-period would have been ruled out. period of 7.9 h for this Hungaria. Subsequent observations and analysis revised this to the half-period of 3.96 h (see Warner, Since the results from 2010 and 2014 favored the 3.2-hour 2011f). The results from the 2014 January observations further solution, the 2007 data were re-examined with the period search confirmed that the shorter period is the right one. confined to 3.000 to 4.000 hours. The result was P = 3.183 h. While several sigmas removed from the other periods, the three 15374 Teta. This was a case where the relatively large amplitude results are now statistically the same. helped overcome noisy data due to the asteroid being V ~ 17.7. The period found here agrees with the one found by the author 4490 Bambery. The period of 5.822 h found from the 2014 January using observations from 2009 (Warner, 2010a). observations compares well against earlier results by the author:

Minor Planet Bulletin 41 (2014) 147

15964 Billgray. A period of 3.571 h was reported from (69406) 1995 SX48. Warner and Stephens (2011d) found a period observations in 2010 (Warner, 2011a). The period of 3.565 h found of 2.2431 h assuming a monomodal lightcurve. Given the four years later is consistent with the earlier result. amplitude of 0.10 mag, this was not an unreasonable assumption. However, the double period of 4.4861 h could not be formally (16562) 1992 AV1. Analysis of observations from 2014 January- excluded. Warner (2014) using observations from 2013 December February found a period of 20.18 h. The asymmetry of the two found the longer period was more likely (P = 4.487 h) and that halves of the lightcurve (and a split halves plot – not shown) rule there was good but not convincing evidence for a satellite. The out a weak solution near 10 hours. In 2011 (Warner, 2011f; 2014 March observations were late in the season and so a 12.251 h), the situation was considerably different. For example, prolonged follow-up campaign to look for a satellite was not the amplitude of the lightcurve was only 0.03 mag, making it on possible. However, they did further support a period of 4.487 h. par with the noise in the data. In such cases, finding a reliable period is very difficult, if not impossible. The new period has been (86217) 1999 TB35. This Hungaria was first observed by the adopted as the correct solution. author in 2010 (Warner, 2011b) when a period of 6.00 h was reported. The 2014 March campaign refined the result to 5.994 (17590) 1995 CG. This Hungaria was first reported to have a hours. period of 16.1 h (Warner, 2012). Analysis of the data set obtained in 2014 February found P = 49.6 h, almost commensurate with an (118337) 1999 BQ9. No previous results were found in the Earth day (as was the 16 h period). This means that one is literature for this Mars-crosser that was observed while waiting for observing almost the same part of the lightcurve at intervals where the moon to clear away from primary targets. an integral multiple of the period equals an integral multiple of 24 hours. In the case of 49.7 hours, this would be every other day. Acknowledgements

The slopes and amplitude of the proposed lightcurve favor Funding for PDS observations, analysis, and publication was adopting the 49-hour period instead of, for example, 24 or 72 provided by NASA grant NNX13AP56G. Work on the asteroid hours. As a result of the most recent analysis, the 2012 data were lightcurve database (LCDB) was also funded in part by National re-examined to look for a longer period. The result is shown in the Science Foundation Grant AST-1210099. second plot for this asteroid. The amplitude is uncertain because no maximum was seen. Here again, one relies on the slopes of the This research was made possible through the use of the AAVSO Fourier lightcurve to serve as a guide, but not one to be taken too Photometric All-Sky Survey (APASS), funded by the Robert critically. Martin Ayers Sciences Fund.

(21688) 1999 RK37. The period from the 2014 campaign agrees References with the one found in 2010 (Warner, 2011a). Behrend, R. (2006, 2007, 2009, 2010) Observatoire de Geneve (44600) 1999 RU10. Warner (2011b) found P = 6.211 h. Almost web site. http://obswww.unige.ch/~behrend/page_cou.html the same period was found in 2014 (P = 6.206 h). It is noteworthy that both times the amplitude was about 1 magnitude even though Brinsfield, J.W. (2008). “The Rotation Periods of 1465 Autonoma, the phase angle bisector longitude differed by about 90 degrees. 1656 Suomi 4483 Petofi, 4853 Marielukac, and (85275) 1994 LY.” This implies that the spin axis of the asteroid favors either the Minor Planet Bul. 35, 23-24. north or south ecliptic pole and not the ecliptic plane. Florczak, M., Dotto, E., Barucci, M.A., Birlan, M., Erikson, A., (48601) 1995 BL. The period from 2010 (Warner, 2011b) and the Fulchignoni, M., Nathues, A., Perret, L., Thebault, P. (1997). most recent observations are in good agreement. As with 1999 “Rotational properties of main belt asteroids: photoelectric and RU10 above, the amplitude was about the same despite PAB CCD observations of 15 objects.” Planet. Space Sci. 45, 1423- longitudes differing by about 70°. 1435.

(49667) 1999 OM2. Previous results include Warner et al. (2011e, Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., 3.48608 h; 2014, 3.487 h). The latter was derived from Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, observations in 2013 December when the phase angle was ~14° H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids and the amplitude 0.46 mag. The 2014 March observations were at 3, 24, 60, 261, and 863.” Icarus 77, 171-186. a phase angle of ~30° and, as expected with increased phase angle, Harris, A.W., Young, J.W., Bowell, E., Tholen, D.J. (1999). the amplitude increased (A = 0.60 mag). The period from the most “Asteroid Lightcurve Observations from 1981 to 1983.” Icarus recent data set was 3.490 h, in good keeping with the earlier 142, 173-201. results. Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., (53530) 2000 AV200. Analysis of data from 2012 (Warner, 2013a) Vilagi, J., Gajdos, S., Carbognani, A.,Hornoch, K., Kusnirak, P., gave ambiguous results. A period of 3.628 h was adopted although Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., periods of 3.374 h and 3.932 h were about as likely. The period Koehn, B.W. (2014). “On the maximum amplitude of harmonics spectrum shown below using the 2014 data shows no ambiguity on an asteroid lightcurve.” Icarus, in press. and, more so, a period of 4.310 h. The data from 2012 can be made to fit to a period of 4.293 h, but it is not a very convincing result. Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). http://www.aavso.org/apass (69142) 2003 FL115. Pravec et al. (2010a) reported a period of 7.389 h for this Hungaria member. The CS3-PDS result from 2014 Higgins, D. (2008). “Asteroid Lightcurve Analysis at Hunters Hill March is in good agreement, despite the lack of coverage for the Observatory and Collaborating Stations: April 2007 - June 2007.” second maximum near 0.80 rotation phase. Minor Planet Bul. 35, 30-32.

Minor Planet Bulletin 41 (2014) 148

Kryszczynska, A., Colas, F., Polinska, M., Hirsch, R., Ivanova, V., Warner, B.D., Pravec, P., Kusnirak, P., Foote, C., Foote, J., Galad, Apostolovska, G., Bilkina, B., Velichko, F.P., Kwiatkowski, T., A., Gajdos, S., Kornos, L., Vilagi, J., Higgins, D., Nudds, S., Yurij, Kankiewicz, P., and 20 coauthors. (2012). “Do Slivan states exist N., Gaftonyuk, N.M. (2006b). “Lightcurves analysis for Hungaria in the Flora family?. I. Photometric survey of the Flora region.” asteroids 3854 George, 4440 Tchantches and 4674 Pauling.” Minor Astron. Astrophys. 546, A72. Planet Bul. 33, 34-35.

Oey, J., Krajewski, R. (2008). “Lightcurve Analysis of Asteroids Warner, B.D. (2007). “Initial Results of a Dedicated H-G from Kingsgrove and Other Collaborating Observatories in the Program.” Minor Planet Bul. 34, 113-119. First Half of 2007.” Minor Planet Bul. 35, 47-48. Warner, B.D. (2008a). “Asteroid Lightcurve Analysis at the Pravec, P., Vokrouhlicky, D., Polishook, D., Scheeres, D.J., Harris, Palmer Divide Observatory: September-December 2007.” Minor A.W., Galad, A., Vaduvescu, O., Pozo, F., Barr, A., Longa, P., and Planet Bul. 35, 67-71. 16 coauthors. (2010). “Formation of asteroid pairs by rotational fission,” Nature 466, 1085-1088. Warner, B.D. (2008b). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: December 2007 - March 2008.” Pravec, P., Scheirich, P., Durech, J., Pollock, J., Kusnirak, P., Minor Planet Bul. 35, 95-98. Hornoch, K., Galad, A., Vokrouhlicky, D., Harris, A.W., Jehin, E., Manfroid, J., Opitom, C., Gillon, M., Colas, F., Oey, J., Vrastil, J., Warner, B.D. (2008c). “Asteroid Lightcurve Analysis at the Reichart, D., Ivarsen, K., Haislip, J., LaCluyze, A. (2014). “The Palmer Divide Observatory: February-May 2008.” Minor Planet tumbling state of (99942) Apophis.” Icarus 233, 48-60 Bul. 35, 163-167.

Pray, D. (2004). “Lightcurve analysis of asteroids 110, 196, 776, Warner, B.D., Harris, A.W., Pravec, P. (2009a). “The Asteroid 804, and 1825.” Minor Planet Bul. 31, 34-36. Lightcurve Database.” Icarus 202, 134-146.

Schober, H.J., Erikson, A., Hahn, G., Lagerkvist, C.-I. (1993). Warner, B.D. (2009b). “Asteroid Lightcurve Analysis at the “Physical Studies of Asteroids. Part XXVI. Rotation and Palmer Divide Observatory: 2008 September-December.” Minor Photoelectric Photometry of Asteroids 323, 350, 582, 1021 and Planet Bul. 36, 70-73. 1866.” Astron. Astrophys. Suppl. Ser. 101, 499-505. Warner, B.D., Higgins, D. (2009c), “Lightcurve Analysis of Shepard, M.K., Clark, B.E., Ockert-Bell, M., Nolan, M.C., Howell, Hungaria Asteroid 4440 Tchantches.” Minor Planet Bul. 36, 90. E.S., Magri, C., Giorgini, J.D., Benner, L.A.M., Ostro, S.J., Harris, A.W., Warner, B.D., Stephens, R.D., Mueller, M. (2010). “A radar Warner, B.D. (2009d). “Asteroid Lightcurve Analysis at the survey of M- and X-class asteroids II. Summary and synthesis.” Palmer Divide Observatory: 2008 December - 2009 March.” Icarus 208, 221-237. Minor Planet Bul. 36, 109-116.

Skiff, B.A. (2011). Warner, B.D. (2009e). “Asteroid Lightcurve Analysis at the ftp.lowell.edu/pub/bas/astlc/5253-2010nov.png Palmer Divide Observatory: 2009 March-June.” Minor Planet Bul. 36, 172-176. Stephens, R.D. (2003). “Photometry of 628 Christine, 754 Malabar, 815 Coppelia, and 1025 Riema.” Minor Planet Bul. 30, Warner, B.D., Stephens, R.D., Harris, A.W., Shepard, M.K. 69-70. (2009f). “Coordinated Lightcurve and Radar Observations of 110 Lydia and 135 Hertha.” Minor Planet Bul. 36, 38-39. Stephens, R.D. (2004). “Photometry of 1196 Sheba, 1341 Edmee, 1656 Suomi, 2577 Litva, and 2612 Kathryn.” Minor Planet Bul. Warner, B.D. (2010a). “Asteroid Lightcurve Analysis at the 31, 95-97. Palmer Divide Observatory: 2009 June-September.” Minor Planet Bul. 37, 24-27. Stephens, R.D., Warner, B.D. (2013). “Lightcurves for 110 Lydia and 1680 Per Brahe.” Minor Planet Bul. 40, 93-94. Warner, B.D. (2010b), “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2010 March – June.” Minor Planet Warner, B.D. (1999). “Asteroid Photometry at the Palmer Divide Bul. 37, 161-165. Observatory.” Minor Planet Bul. 26, 31-33. Warner, B.D. (2011a). “Lightcurve Analysis at the Palmer Divide Warner, B.D. (2005a). “Lightcurve analysis for asteroids 242, 893, Observatory: 2010 June-September.” Minor Planet Bul. 38, 25-31. 921, 1373, 1853, 2120, 2448 3022, 6490, 6517, 7187, 7757, and 18108.” Minor Planet Bul. 32, 4-7. Warner, B.D. (2011b). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2010 September-December.” Minor Warner, B.D. (2005b). “Asteroid lightcurve analysis at the Palmer Planet Bul. 38, 82-86. Divide Observatory - fall 2004.” Minor Planet Bul. 32, 29-32. Warner, B.D., Pravec, P., Kusnirak, P., Harris, A.W., Cooney Jr., Warner, B.D., Pravec, P., Kusnirak, P., Cooney Jr., W., Gross, J., W.R., Gross, J., Terrell, D., Nudds, S., Vilagi, J., Gadjdos, S., Terrell, D., Nudds, S. (2005c). “(3309) Brorfelde.” CBET 279. Masi, G., Pray, D.P., Dyvig, R., Reddy, V. (2011c). “Lightcurves from the Initial Discovery of Four Hungaria Binary Asteroids.” Warner, B.D., Pray, D.P., Dyvig, R., Reddy, V. (2006a). Minor Planet Bul. 38, 107-109. “Lightcurve for Hungaria asteroid 1600 Vyssotsky over several apparitions.” Minor Planet Bul. 33, 45-46. Warner, B.D., Stephens, R.D. (2011d). “Lightcurve Analysis for a Trio of Asteroids.” Minor Planet Bul. 38, 110-111.

Minor Planet Bulletin 41 (2014) 149

Warner, B.D., Galad, A., Veres, P., Pravec, P., Kusnirak P. (2011e). “Lightcurve Analysis of Hungaria Asteroid (49667) 1999 OM.” Minor Planet Bul. 38, 103.

Warner, B.D. (2011f). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2010 December- 2011 March.” Minor Planet Bul. 38, 142-149

Warner, B.D., Pravec, P., Kusnirak, P., Gajdos, S., Veres, P., Kornos, L., Harris, A.W. (2011g). “Lightcurve Analysis of Hungaria Asteroid 4464 Vulcano.” Minor Planet Bul. 38, 168-169.

Warner, B.D. (2012). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2012 March – June.” Minor Planet Bul. 39, 245-252.

Warner, B.D. (2013a). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2012 June - September.” Minor Planet Bul. 40, 26-29.

Warner, B.D. (2013b). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2012 September - 2013 January.” Minor Planet Bul. 40, 71-80.

Warner, B.D. (2014). “Asteroid Lightcurve Analysis at CS3- Palmer Divide Station: 2013 September-December.” Minor Planet Bul. 41, 102-112.

Minor Planet Bulletin 41 (2014) 150

Minor Planet Bulletin 41 (2014) 151

Minor Planet Bulletin 41 (2014) 152

Minor Planet Bulletin 41 (2014) 153

Minor Planet Bulletin 41 (2014) 154

Minor Planet Bulletin 41 (2014) 155

by MPO Canopus. Because of the large number of data points, the data for the lightcurves presented here have been binned in sets of three points with a maximum time interval between points no greater than 5 minutes.

18 Melpomene. Warner et al. (2014) state a secure synodic rotation period of 11.570 hours based on several consistent published values. New observations were obtained on two nights 2014 Jan. 15 and 21 to assist in lightcurve inversion modeling. It must be recognized that observations on only two nights separated by many rotational cycles provide equally good fits to trial lightcurves at several different periods which may be found as minima on the period spectrum. One of these minima, at 11.571 ± 0.002 hours, was very near the accepted period. The lightcurve presented here is phased to this value with amplitude 0.16 ± 0.02 magnitudes and full phase coverage. 234 Barbara. Previously published periods are by Schober (1981), 26.5 hours; Behrend (2010), 26.468 hours; and Hamanowa (2011), 26.463 hours. New observations on 9 nights 2013 Dec. 31 - 2014 Feb. 25 provide a good fit to a lightcurve phased to 26.473 ± 0.002 hours with amplitude 0.16 ± 0.02 magnitudes. This is fully consistent with previous determinations.

236 Honoria. Previously published periods are by Behrend (2006), 16.8 hours; Behrend (2007), 17. hours; and Harris and Young (1989), 12.333 hours. New observations on 7 nights 2014 Jan. 3 - Feb. 19 provide a good fit to a lightcurve phased to 12.336 ± 0.001 hours with amplitude 0.23 ± 0.02 magnitudes. This is consistent with Harris and Young (1989) and rules out all other published periods.

520 Franziska. The only previously published period is by Binzel (1987) of 14.0 hours based on a sparse lightcurve. New observations on 7 nights 2013 Dec. 11 - 2014 Jan. 19 provide a LIGHTCURVES AND DERIVED ROTATION PERIODS good fit to a lightcurve phased to 16.507 ± 0.001 hours with FOR 18 MELPOMENE, 234 BARBARA, 236 HONORIA, amplitude 0.35 ± 0.02 magnitudes. This rules out the 14 hour 520 FRANZISKA, AND 525 ADELAIDE period by Binzel (1987).

Frederick Pilcher 525 Adelaide. Warner et al. (2014) report no previous period 4438 Organ Mesa Loop determinations. A single session 2009 Oct. 23 at celestial Las Cruces, NM 88011-8403 USA longitude 57 degrees, celestial latitude -4 degrees and not [email protected] previously published featured a barely detectable increase of 0.02 magnitudes in 8 hours. Additional observations on 8 nights 2014 (Received: 28 March) Feb. 12 - Mar. 27 provide a good fit to a lightcurve phased to 19.967 ± 0.001 hours with amplitude 0.35 ± 0.03 magnitudes. Use of the amplitude aspect method of finding the rotational pole From new lightcurves obtained near their 2014 suggests that one of the two rotational poles lies within a few oppositions rotation periods and amplitudes are found for degrees of celestial longitude 57 degrees and latitude -4 degrees. 18 Melpomene 11.571 ± 0.002 hours, 0.16 ± 0.02 magnitudes; 234 Barbara 26.473 ± 0.002 hours, References amplitude 0.16 ± 0.02 magnitudes; 236 Honoria 12.336 ± 0.001 hours, 0.23 ± 0.02 magnitudes; 520 Franziska Behrend, R. (2006). Observatoire de Geneve web site. 16.507 ± 0.001 hours, 0.35 ± 0.02 magnitudes; and 525 http://obswww.unige.ch/~behrend/page_cou.html. Adelaide 19.967 ± 0.001 hours, amplitude 0.35 ± 0.03 magnitudes near celestial longitude 180 degrees and 0.02 Behrend, R. (2007). Observatoire de Geneve web site. ± 0.01 magnitudes at celestial longitude 57 degrees, http://obswww.unige.ch/~behrend/page_cou.html. latitude -4 degrees. The amplitude - aspect method strongly suggests the latter position lies within a few Behrend, R. (2010). Observatoire de Geneve web site. degrees of one of the two rotational poles. http://obswww.unige.ch/~behrend/page_cou.html.

Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids.” All observations reported here were made at the Organ Mesa Icarus 72, 135-208. Observatory using a Meade 35-cm LX-200 GPS Schmidt- Cassegrain (SCT), SBIG STL-1001E CCD, red filter for bright 18 Hamanowa, H. (2011). Melpomene, clear filter for the other targets. Exposures were http://www2.ocn.ne.jp/~hamaten/astlcdata.htm unguided. Image measurement and lightcurve analysis were done Minor Planet Bulletin 41 (2014) 156

Harris, A.W., Young, J.W. (1989) “Asteroid Lightcurve Observations from 1979-1981.” Icarus 81, 314-364.

Schober, H.J. (1981). “Rotation period of 234 Barbara, a further slowly spinning asteroid.” Astron. Astrophys. 96, 302-305.

Warner, B.D., Harris, A.W., Pravec, P. (2014). “Asteroid Lightcurve Data File, March 1, 2014.” http://www.minorplanet.info/lightcurvedatabase.html

Minor Planet Bulletin 41 (2014) 157

LIGHTCURVE ANALYSIS FOR 2713 LUXEMBOURG lightcurve indicates an amplitude of A = 0.57 mag and an unambiguous period of P = 3.581 ± 0.002 h, which is consistent Emily A. Mailhot and Alan H. Midkiff with the Bernasconi value. Visual inspection of the different Star View Hill Education Center (W66) nights’lightcurves suggests that the relative brightness of the 120 Camp Wasigan Road minima change over the range of solar phase angles observed. Blairstown, NJ 07825 USA [email protected] Acknowledgements

(Received: 31 March) We acknowledge two Web sites that we found useful for our work: the MPO One Asteroid Info Database Search Engine at (http://www.minorplanet.info/PHP/OneAsteroidInfo.php), and the Photometric observations of Koronis family asteroid 2013 version of the Slivan “Koronis Family Asteroid Rotation 2713 Luxembourg were made over five nights during Lightcurve Observing Program” (http://koronisfamily.com). 2013 November-December. The lightcurve shows a synodic period P = 3.582 ± 0.002 h with amplitude A = References 0.57 mag. Bernasconi, Laurent. “(2713) Luxembourg.” http://translate.google.com/translate?hl=en&sl=fr&u=http://obsw Observations of the asteroid 2713 Luxembourg were conducted at ww.unige.ch/~behrend/page_cou.html the Star View Hill Education Center using a 0.6-m f/4.9 unfolded JMI NTT Newtonian reflecting telescope in combination with an Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., FLI CCD camera. The FLI camera has a 512x512 array of 16- Poutanen, M., Scarltriti, F., Zappala, V., Schoer, H.J., Debehogne, micron pixels resulting in an image scale of 1.3 arcsecond per H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, pixel. All images were guided, unfiltered, and unbinned. Exposures 24, 60, 261, and 863.” Icarus 77, 171-186. were 60 seconds, taken primarily at –20°C. All images were Slivan, S.M. (2002). “Spin vector alignment of Koronis family calibrated and reduced with dark and flat-field frames using MPO asteroids.” Nature 419, 49-51. Canopus (Warner, 2012). Additionally, processed images were measured with MPO Canopus using a differential photometry Slivan, S.M. (2012). “Epoch Data in Sidereal Period technique. Comparison stars in the image field having near-solar Determination. I. Initial Constraint from Closest Epochs.” Minor colors were chosen with the program’s “comp star selector” Planet Bulletin 39, 204-206. feature. Vokrouhlicky, D., Nesvorny, D., Bottke, W.F. (2003). “The vector 2713 Luxembourg is a 14.9-km Koronis family main-belt asteroid. alignments of asteroid spins by thermal torques.” Nature 425, 147- Koronis members were possibly formed by a collision of two 151. larger bodies over two billion years ago. Analysis of their rotational lightcurves has revealed that the spin vector orientations Warner, B.D. (2012). MPO Software, MPO Canopus version of several of the largest Koronis family asteroids are unexpectedly 10.4.1.12. Bdw Publishing, Eaton, CO. aligned in obliquity (Slivan, 2002), which has led to the suggestion that thermal effects might be responsible (Vokrouhlicky et al., 2003). Prior lightcurve analysis of the asteroid was completed by Bernasconi in 2006 (unpublished) resulting in a period of 3.579 ± NEAR-EARTH ASTEROID LIGHTCURVE ANALYSIS AT 0.002 h. Further lightcurve observations are important because spin CS3-PALMER DIVIDE STATION: vector analysis requires data from several apparitions (Slivan, 2014 JANUARY-MARCH 2012). Brian D. Warner Center for Solar System Studies / MoreData! 446 Sycamore Ave. Eaton, CO 80615 USA [email protected]

(Received: 31 March)

Lightcurves for 40 near-Earth asteroids (NEAs) were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2014 January through March.

CCD photometric observations of 40 near-Earth asteroids were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2014 January through March. Table I gives a listing Period analysis was carried out using MPO Canopus and the Harris of the telescope/CCD camera combinations used for the Fourier analysis feature (Harris et al., 1989). The resulting doubly- observations. All the cameras use the same CCD chip from the periodic lightcurve contains 968 data points obtained over five Kodak KAF blue-enhanced family and so have essentially the nights during the period 2013 November-December. The Minor Planet Bulletin 41 (2014) 158 same response. The pixel scales for the combinations range from through crowded star fields and so a large number of data points 1.24-1.60 arcsec/pixel. were rejected due to interference from field stars. Even so, the nightly zero points required a minimum of adjustment (<0.05 Desig Telescope Camera mag). No amount of zero point adjustments allowed a believable PDS-1-12N 0.30-m f/6.3 Schmidt-Cass ML-1001E solution near 7.5 hours. PDS-1-14S 0.35-m f/9.1 Schmidt-Cass FLI-1001E PDS-2-14N 0.35-m f/9.1 Schmidt-Cass STL-1001E 4954 Eric. The period of 12.058 h found from CS3-PDS data PDS-2-14S 0.35-m f/9.1 Schmidt-Cass STL-1001E PDS-20 0.50-m f/8.1 Ritchey-Chretien FLI-1001E agrees with those previously reported by Krugly (1994, 12.065 h), Table I. List of CS3-PDS telescope/CCD camera combinations. Pravec et al. (1995, 12.056 h), and Zeigler et al. (1998, 12.057 h).

All lightcurve observations were unfiltered since a clear filter can (25916) 2001 CP44. Elenin et al. (2012) reported a period of 4.19 result in a 0.1-0.3 magnitude loss. Guiding was done on a field ± 0.01 h based on data from three consecutive nights in 2010. The star, which sometimes resulted in a trailed image for the asteroid. CS3-PDS data were in two blocks of consecutive nights with a The exposure duration varied depending on the asteroid’s one-day gap between blocks. Analysis of the CS3-PDS data found brightness and sky motion. P = 3.871 h. It is noteworthy that the two periods differ by almost exactly one-half rotation over a period of 24 hours. In the case of a Measurements were done using MPO Canopus. If necessary, an highly symmetrical lightcurve, this leads to the possibility of a elliptical aperture with the long axis parallel to the asteroid’s path “rotational alias”. The Elin et al. curve is symmetrical; however was used. The Comp Star Selector utility in MPO Canopus finds the individual runs covered at least one-half of a bimodal up to five comparison stars of near solar-color to be used in lightcurve, which diminishes the chances of finding an aliased differential photometry. Catalog magnitudes are usually taken from period. While the individual runs of the CS3-PDS data do not have the MPOSC3 catalog, which is based on the 2MASS catalog such coverage, the resulting lightcurve is not symmetrical. (http://www.ipac.caltech.edu/2mass) but with magnitudes Attempts to force the CS3-PDS data to the longer period produced converted from J-K to BVRI using formulae developed by Warner unsatisfactory results. For now, the Elenin et al. period should be (2007). When possible, magnitudes are taken from the APASS considered to be the more likely answer. catalog (Henden et al., 2009) since these are derived directly from reductions based on Landolt standard fields. Using either catalog, (35107) 1991 VH. This is a known binary (Pravec et al., 2006; the nightly zero points have been found to be consistent to about Vander Haagen, 2010). The orbital period of the satellite, ±0.05 magnitude or better, but on occasion are as large as 0.1 mag. determined by mutual events (occultations and/or eclipses) is about This consistency is critical to analysis of long period and/or 32.4 ± 0.3 hours. Pravec et al. (2006) also reported a tertiary period tumbling asteroids. Period analysis is also done using MPO of 12.836 h, possibly due to the rotation of a second satellite. The Canopus, which implements the FALC algorithm developed by dual period feature of MPO Canopus was used to look for Harris (Harris et al., 1989). evidence of these periods in the CS3-PDS data.

In the plots below, the “Reduced Magnitude” is Johnson V (or After several iterations where two of three periods were subtracted Cousins R) as indicated in the Y-axis title. These are values that to find the third period, the result was a period for the primary of have been converted from sky magnitudes to unity distance by P1 = 2.623 ± 0.002 h, in agreement with previous results. The “P2: applying –5*log (rΔ) to the measured sky magnitudes with r and Δ No sub P3” plot shows the results of subtracting only P1. The “P3” being, respectively, the Sun-asteroid and Earth-asteroid distances plot shows the final result for the tertiary period: P3 = 11.73 h. This in AU. The magnitudes were normalized to the phase angle given is considerably different from the value reported by Pravec et al. in parentheses, e.g., alpha(6.5°), using G = 0.15, unless otherwise (2006) and is likely due to not having enough data to cover all stated. The horizontal axis is the rotational phase and ranges from three periods throughout a cycle. The “P2: Sub P3” plot reveals –0.05 to 1.05. what is possibly the rotation of the first satellite but no events. The period of P2 = 32.15 h is in general agreement with the previously For the sake of brevity, only some of the previously reported reported values. results may be referenced in the discussions on specific asteroids. For a more complete listing, the reader is directed to the asteroid The P2 and P3 results should viewed with a suspicious eye. Their lightcurve database (LCDB; Warner et al., 2009). The on-line primary value is that they help produce a primary period in good version at http://www.minorplanet.info/lightcurvedatabase.html agreement with results using more extensive data sets. allows direct queries that can be filtered a number of ways and the (40267) 1999 GJ4. Earlier results for this NEA include Galad results saved to a text file. A set of text files of the main LCDB (2005, 4.95692 h) and Polishook (2012, 4.97 h). There are two tables, including the references with bibcodes, is also available for plots for 1999 GJ4 based on CS3-PDS data. The first is from 2014 download. When possible, researchers are strongly to obtain the January and the second from 2014 February. In January, the original references listed in the LCDB for their work. parameters were P = 4.959 ± 0.005 h, A = 0.94 ± 0.03 mag. A Individual Results month later the values were P = 4.953 ± 0.002 h, A = 0.86 ± 0.02 mag. The more notable change was in the amplitude. In January, 1943 Anteros. Pravec et al. (1988) reported a period of 2.8695 h the solar phase angle was ~33.5° while in February it was ~7°, so it for this NEA. The result of analysis from the observations at CS3- was to be expected that the amplitude would be less in February. PDS in 2013 December is consistent with that earlier result. The average value of the lightcurves from the two data sets was 4055 Magellan. Pravec et al. (2000) found a period of P = 7.475 h used to find the absolute magnitude, H = 16.05 ± 0.05, and phase based on observations in 2000. The period spectrum using the slope parameter, G = 0.42 ± 0.05. Pravec et al. (2012) found H = CS3-PDS data from 2014 shows a weak solution near that value 16.08 ± 0.21 and G = 0.5 ± 0.2. The value for G is consistent with but, more so, that a period of 6.384 h is a considerably better fit. a high albedo, i.e., pV ~ 0.43 (Warner et al., 2009). This is The somewhat sparse data set is the result of the asteroid moving supported by the results from the WISE survey (Mainzer et al., Minor Planet Bulletin 41 (2014) 159

2014 Number Name mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 1943 Anteros *12/23-12/30 331 29.7,27.4 125 -11 2.867 0.001 0.10 0.01 4055 Magellan 01/26-02/01 74 13.5,14.6 113 -23 6.38 0.05 0.68 0.05 4954 Eric 01/26-03/05 353 27.4,11.0 183 2 12.057 0.001 0.80 0.03 25916 2001 CP44 03/16-03/20 67 37.2,37.8 246 14 3.871 0.002 0.35 0.03 35107 1991 VH 02/09-02/20 312 40.2,35.4 179 11 2.623 0.002 0.10 0.02 40267 1999 GJ4 01/18-01/23 159 34.8,31.4 168 3 4.959 0.005 0.94 0.02 ”” ”” 02/24-02/26 237 7.2,7.0 159 10 4.953 0.002 0.86 0.02 53435 1999 VM40 02/14-02/15 241 21.3,21.4 127 24 5.172 0.006 0.20 0.02 68031 2000 YK29 01/21-01/29 170 38.6,36.0 153 9 4.48 0.05 0.05 0.01 85990 1999 JV6 01/28-02/02 413 16.6,8.0 138 3 6.538 0.001 0.87 0.03 86039 1999 NC43 03/15-03/20 62 65.3,59.7 125 -7 34 2 0.60 0.10 138127 2000 EE14 03/07-03/09 132 77.6,77.9 197 40 2.586 0.005 0.26 0.02 143409 2003 BQ46 03/08-03/14 241 29.5,27.9 195 6 10.531 0.005 1.14 0.03 243566 1995 SA 03/12-03/19 230 52.6,64.9 135 -8 14.37 0.02 0.21 0.03 275677 2000 RS11 03/16 123 73.9 209 23 4.3 0.2 1.37 0.02 ”” ”” 03/17 144 70.2 206 25 4.38 0.06 1.25 0.03 ”” ”” 03/16-03/17 267 73.9,70.2 208 24 4.445 0.002 1.30 0.03 277570 2005 YP180 02/01-02/02 217 18.9,16.5 141 -8 3.689 0.005 0.27 0.02 294739 2008 CM 01/13-01/17 295 71.1,67.4 68 -6 3.054 0.001 0.48 0.03 357622 2005 EY95 03/12-03/15 476 56.3,40.5 185 24 3.925 0.005 0.24 0.03 377097 2002 WQ4 01/03-01/07 56 11.4,13.1 80 -8 36 3 0.6 0.1 1995 CR 02/20-02/20 404 31.9,31.9 148 16 2.66 0.04 0.16 0.03 2006 DP14 02/22-02/23 119 29.0,29.1 136 -9 5.77 0.01 1.05 0.03 2009 CT 02/21-03/05 188 15.2,35.7 141 -8 42 0.2 0.63 0.03 2009 QF31 02/23-02/24 139 13.6,12.9 164 -4 4.840 0.005 0.75 0.03 2011 BT15 01/10-01/11 232 53.8,50.6 139 2 0.109138 0.000002 0.61 0.03 2012 AU10 01/26-01/29 158 29.4,29.2,29.3 107 -11 10.45 0.05 0.20 0.02 2013 XV8 01/02-01/11 260 22.9,18.6 119 1 9.23 0.02 0.09 0.02 2013 YZ13 01/02-01/07 572 19.6,6.0 108 8 23.86 0.01 0.93 0.03 2013 PD21 02/01-02/09 559 26.1,20.5 148 7 4.81 0.01 0.13 0.02 2013 XF22 01/23-01/23 121 13.8,13.8 112 -6 7.63 0.01 0.29 0.03 2013 YZ37 01/23-01/29 152 22.2,20.1 143 -1 8.87 0.01 0.18 0.03 2013 WT44 03/21-03/28 879 16.4,12.7,21.7 190 +1 2.8849 0.0006 0.05 0.01 2014 CR 02/22-02/22 631 51.4,51.4 146 26 5.9 0.2 0.51 0.03 2014 EM 03/12-03/13 677 4.0,15.1 176 -3 2.963 0.005 0.46 0.05 2014 BR8 02/01-02/04 153 23.9,28.8 125 -13 13.85 0.05 0.80 0.05 2014 CG13 02/17-02/20 278 17.3,21.6 139 0 24.5 0.2 0.85 0.10 2014 CU13 03/07-03/09 619 27.9,43.9 182 12 14.36 0.02 0.45 0.03 2014 EY24 03/19 243 21.5 185 10 - - - - 2014 AY28 02/25-02/26 146 17.6,17.1 161 -9 0.9139 0.0002 0.54 0.02 2014 EL45 03/14-03/15 521 0.0,19.9 124 3 5.49 0.005 0.51 0.03 2014 BR57 02/17-02/18 279 39.5,48.7 144 22 5.07 0.02 0.30 0.03 2014 DX110 03/05-03/05 263 32.5,32.5 149 5 0.12041 0.00008 0.37 0.02 Table II. Observing circumstances. An asterisk before the dates indicates the observations started or were entirely in 2013. 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, unless two values are given (first/last date in range).

2011), which reported pV = 0.453. The CS3-PDS values give a of 4.48 hours. This was one of numerous, nearly equal solutions in diameter of D = 1.30 ± 0.05 km. WISE gave D = 1.64 ± 0.05 km. the period spectrum and cannot be considered more than a guess.

(53435) 1999 VM40. The CS3-PDS result from 2014 February (85990) 1999 JV6. No previous results could be found in the was P = 5.172 ± 0.006 h, in good agreement with results from literature for this NEA. The large amplitude and extended data set Pravec et al. (2000) and Warner (2014). The data from Warner make the solution secure. (2014) were combined with the more recent data set to find H = 14.50 ± 0.15, G = 0.04 ± 0.07. Pravec et al. (2012) found H = (86039) 1999 NC43. Pravec et al. (2000) reported two possible 14.91 ± 0.08, G = 0.20 ± 0.04. Since the value for H is dependent but significantly different periods for 1999 NC43. The shorter on the area of the asteroid’s profile projected onto the sky, this period, P = 34.49 h, is loosely supported by the sparse data set could account for some of the difference. However, a more likely obtained at CS3-PDS in 2014 March. The long period from Pravec cause is the lack of data below 10° phase angle. H-G analysis using et al. was 122 h, which was not supported by the 2014 data. data at only larger phase angles usually produces a too bright (lower) value for H. (138127) 2000 EE14. The period of 2.586 h is considered secure. The period and amplitude make the asteroid a potential binary (68031) 2000 YK29. Despite having data from five nights in 2014 candidate. No signs of mutual events or a secondary period were January, no definitive period could be found. The night-to-night detected. zero points were consistent to <0.05 mag, removing any justification for manipulating them beyond very small amounts (143409) 2003 BQ46 and (243566) 1995 SA. No previous results during period analysis. The plot shows the data forced to a period were found in the literature. Minor Planet Bulletin 41 (2014) 160

(275677) 2000 RS11. Three plots are presented for this asteroid showed the primary to be nearly spheroidal, which would produce which was only 0.05 AU from Earth in mid-March 2014. On a low amplitude lightcurve even with a more equatorial view. March 16, the synodic period was 4.3 ± 0.2 h and amplitude 1.37 mag. For the next night, which provided more complete coverage 2014 CR. Hicks et al. (2014b) observed this asteroid on the same of the unusually shaped lightcurve, the parameters were P = 4.38 ± night as CS3-PDS. They found a period of 6.35 hours. This 0.06 h and A = 1.25 ± 0.03 mag. The combined data set (third plot) solution is a little more reliable than the one of 6.6 ± 0.3 h found gave P = 4.444 ± 0.001 h and A = 1.31 ± 0.03 mag. Close using the CS3-PDS data. The somewhat large uncertainty is due to inspection of the combined lightcurve shows the slight evolution of the break in coverage at the minimum near 0.7 rotation phase and the lightcurve’s shape from the first to second night, especially immediately following maximum. near 0.3 rotation phase. 2014 EM. This is a good example of being able to find a solution (277570) 2005 YP180, (294739) 2008 CM, and (357622) 2005 with noisy data by overwhelming the analysis engine with a large EY95. No previous results were found in the literature. number of data points, almost 700 in this case. Fortunately, the amplitude of 0.46 mag was significantly more than the error bars (377097) 2002 WQ4. This asteroid was chosen because it was of the individual data points. available at the beginning of the night and so could be worked until a secondary target had risen high enough in the east. When 2014 BR8. The diameter of this NEA is about 140 meters. As such, choosing such a target, one is betting that the rotation period is the odds are normally in favor of it being a superfast rotator, i.e., short enough to be readily covered, or nearly so, with an observing with P < 2 hours (Statler et al., 2013). Therefore, the period of run of only 2-5 hours. In this case, “the house won.” After three 13.85 h was somewhat unexpected. The estimated tumbling nights in 2014 January, it was apparent that it would not be damping time for this period is at least the age of the Solar System possible for a single station to get enough data to find a reliable (Pravec et al., 2014, and reference therein). However, there were solution. Even so, the slopes of the two longer nights fit the Fourier no obvious signs that the asteroid was in a state of non-principal curve well and so the period of 36 hours is likely with 50% of the axis rotation. true period. 2014 CU13. The period spectrum favors a period of 14.36 h but the 1995 CR. Note that the 404 data points were obtained on a single data can be made to fit to one degree or another with periods of night. Fortunately, the observing run covered almost two full 9.63 and 17.57 hours. A review of the plot for the shorter period cycles of the stated period of 2.66 hours. shows a significant problem near 0.3-0.4 rotation phase. The plot for the longest period shows a gap near 0.65 rotation phase which 2006 DP14. Hicks et al. (2014a) observed this NEA five days could be due to the Fourier analysis finding a minimum RMS before CS3-PDS. They found P = 5.78 h and A = 0.90 mag. The value by minimizing the number of overlapping data points (a “fit CS3-PDS data produced P = 5.77 h and A = 1.05 mag. Radar by exclusion”). In all three cases, the trimodal lightcurve raises observations on 2014 February 11 supported a period of about 6 some doubts. Even at nearly 30° phase angle, a bimodal lightcurve hours and a diameter of 400 meters (Radar team, 2014). can be expected for an amplitude of 0.45 mag, though not absolutely required. It may be of interest that the product of any 2009 CT, 2009 QF31, 2011 BT15, and 2012 AU10. No previous two periods is nearly an integral multiple of the remaining period. results were found in the literature. This may be an indication that the asteroid is in a tumbling condition. However, the total span of the data set is too short to 2013 XV8. This was another asteroid that produced no definitive allow a proper analysis for that possibility. solution, as seen from the period spectrum that shows mostly flat line noise, save a slight minimum at 9.23 hours. The plot showing 2014 EY24. This NEA was observed on one night. The raw data the data forced to this period is not overly convincing. from the run are shown in the plot. Period analysis from 0.001 to 10 hours resulted in a period spectrum that was a flat line with low 2013 YZ13. Despite the data covering only a small portion of a level noise. complete lightcurve, the period of 23.86 hours is fairly secure. First, given the amplitude of almost a full magnitude and phase 2014 AY28 and 2014 EL45. No previous results were found in the angle < 20°, it’s virtually certain that the full lightcurve is bimodal literature. (Harris et al., 2014). As such, the rise from a minimum to the following maximum should take about 0.25 of the rotation period, 2014 BR57. The plot shows the data fit to a period of 5.07 hours, as is the case for 2013 YZ13. Data from a station well separated in but there’s little reason to consider it the correct value. longitude would have been extremely beneficial. 2014 DX110. Despite an amplitude of 0.37 mag, it’s not certain if 2013 PD21. As seen in the period spectrum, the period of 4.82 the lightcurve should be monomodal (0.06019 h) or bimodal hours hardly stands out from two others, one on each side of the (0.12041 h). A close look at the plot for the longer period shows chosen minimum. From left to right, the three nearly equal periods that the two halves of the curve are nearly identical. This is represent 6, 5, and 4 rotations per Earth day. supported in the “split halves” plot based on the longer period which shows a slight misalignment near 0.2/0.7 rotation phase. 2013 XF22 and 2013 YZ37. No previous results were found in the This favors, if only a little, that the longer period is the right literature. solution. However, it is too little to be certain.

2013 WT44. Radar observations (Lance Benner, private The specialized “split halves” plot was taken from Harris et al. communications) showed this to be a binary asteroid. The viewing (2014). Here, the full period (P) is used but the data are plotted aspect was likely close to pole-on during the time of the CS3-PDS using the half-period (P/2). This results in the second half of the observations and so no mutual events were possible. The lightcurve overlaying the first half. In the plot below, open black lightcurve showed no signs of a secondary period. Radar also (dark) circles represent data from 0.0 to 0.5 rotation phase of the

Minor Planet Bulletin 41 (2014) 161 full period. Red (lighter) stars represent data from 0.5 to 1.0 Pravec, P., Wolf, M., Sarounova, L. (1998). “Lightcurves of 26 rotation phase. If the two halves are essentially identical, then there Near-Earth Asteroids.” Icarus 136, 124-153. is a possibility for the half-period being the correct solution. If the two halves diverge significantly, the half-period is ruled out. Pravec, P., Harris, A.W., Scheirich, P., Kušnirák, P., Šarounová, L., Hergenrother, C.W., Mottola, S., Hicks, M.D., Masi, G., Acknowledgements Krugly, Yu.N., Shevchenko, V.G., Nolan, M.C., Howell, E.S., Kaasalainen, M., Galád, A., Brown, P., Degraff, D.R., Lambert, Funding for PDS observations, analysis, and publication was J.V., Cooney, W.R., Foglia, S. (2005). “Tumbling asteroids.” provided by NASA grant NNX13AP56G. Work on the asteroid Icarus 173, 108-131. lightcurve database (LCDB) was also funded in part by National Science Foundation Grant AST-1210099. Pravec, P., Scheirich, P., Durech, J., Pollock, J., Kusnirak, P., Hornoch, K., Galad, A., Vokrouhlicky, D., Harris, A.W., Jehin, E., This research was made possible through the use of the AAVSO Manfroid, J., Opitom, C., Gillon, M., Colas, F., Oey, J., Vrastil, J., Photometric All-Sky Survey (APASS), funded by the Robert Reichart, D., Ivarsen, K., Haislip, J., LaCluyze, A. (2014). “The Martin Ayers Sciences Fund. tumbling state of (99942) Apophis.” Icarus 233, 48-60.

References Radar Team (2014). http://www.jpl.nasa.gov/news/news.php?release=2014-060 Galad, A., Pravec, P., Kusnirak, P., Gajdos, S., Kornos, L., Vilagi, J. (2005). “Joint Lightcurve Observations of 10 Near-Earth Statler, T.S., Cotto-Figueroa, D., Riethmiller, D.A., Sweeney, Asteroids from Modra and Ondrejov.” EM&P 97, 147-163. K.M. (2013). “Size matters: The rotation rates of small near-Earth asteroids.” Icarus 225, 141-155. Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Vander Haagen, G. (2010). “(35107) 1991 VH: An Apollo Binary H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids Asteroid.” Minor Planet Bul. 37, 36. 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Warner, B.D. (2007). “Initial Results of a Dedicated H-G Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Program.” Minor Planet Bul. 34, 113-119. Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Warner, B.D. (2014). “Near-Earth Asteroid Lightcurve Analysis at Koehn, B.W. (2014). “On the maximum amplitude of harmonics CS3-Palmer Divide Station: 2013 September-December.” Minor on an asteroid lightcurve.” Icarus, in press. Planet Bul. 41, 113-124. http://dx.doi.org/10.1016/j.icarus.2014.03.004 Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Hicks, M., Ebelhar, S.. (2014a). Astronomer's Telegram 5928. Lightcurve Database.” Icarus 202, 134-146. http://www.astronomerstelegram.org Zeigler, K.W., Monsees, R.D., Brown, L. (1998). “CCD Hicks, M., Frederick, J., Harley, I. (2014b). Astronomer's Photometry of Asteroids 2270 Yazhi, 4954 Eric, and (5534) 1941 Telegram 5801. http://www.astronomerstelegram.org UN.” Minor Planet Bul. 25, 13-14.

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

Krugly, Yu.N., Shevchenko, V.G. (1994). Abstracts of Small Bodies Conf., Mariehamn, p. 86.

Mainzer, A., Grav, T., Masiero, J., Hand, E., Bauer, J., Tholen, D., McMillan, R.S., Spahr, T., Cutri, R.M., Wright, E., Watkins, J., Mo, W., Maleszewski, C. (2011). “NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results.” Astrophys. J. 741, A90.

Mottola, S., De Angelis, G., Di Martino, M., Erikson, A., Hahn, G., Neukum, G. (1995). “The near-earth objects follow-up program: First Results.” Icarus 117, 62-70.

Polishook, D. (2012). “Lightcurves and Spin Periods of Near-Earth Asteroids, The Wise Observatory, 2005-2010.” Minor Planet Bul. 39, 187-192.

Pravec, P., Wolf, M., Varady, M., Barta, P. (1995a). “CCD Photometry of 6 Near-Earth Asteroids.” EM&P 71, 177-187.

Pravec, P.,Wolf, M., Sarounova, L. (1995b, 2000). http://www.asu.cas.cz/~ppravec/neo.htm

Minor Planet Bulletin 41 (2014) 162

Minor Planet Bulletin 41 (2014) 163

Minor Planet Bulletin 41 (2014) 164

Minor Planet Bulletin 41 (2014) 165

Minor Planet Bulletin 41 (2014) 166

Minor Planet Bulletin 41 (2014) 167

Minor Planet Bulletin 41 (2014) 168

Minor Planet Bulletin 41 (2014) 169

ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY was tried at 12.255; a slight fit was found at 12.33 h, but was not as SOUTHERN SKY OBSERVATORY: 2013 OCTOBER good as the fit at 9.824 h.

Rachel Vinson, Robert Moore, Richard Ditteon 3062 Wren: The rotational period found is close, but does not lie Rose-Hulman Institute of Technology, CM 171 within the range of uncertainty reported in Behrend (2006): 6.967 5500 Wabash Avenue, Terre Haute, IN 47803 ± 0.007 h. It does agree with the value reported in Carbo et al. [email protected] (2009): 7.097 ± 0.003h.

(Received: 4 April) References

Behrend, R. (2006). Observatoire de Geneve web site. Photometric data for seven asteroids were collected over http://obswww.unige.ch/~behrend/page_cou.html the course of six nights in 2013 October. The asteroids were: 1359 Prieska, 1384 Kniertje, 2161 Grissom, Behrend, R. (2007). Observatoire de Geneve web site. 3062 Wren, 6043 Aurochs, (22412) 1995 UQ4, and http://obswww.unige.ch/~behrend/page_cou.html (24393) 2000 AG 183. Carbo, L., Green, D., Kragh, K., Krotz, J., Meiers, A., Patino, B., Pligge, Z., Shaffer, N., Ditteon, R. (2009). “Asteroid Lightcurve Seven asteroids were remotely observed from the Oakley Southern Analysis at the Oakley Southern Sky Observatory: 2008 October Sky Observatory in New South Wales, Australia. These Thru 2009 March.” Minor Planet Bulletin 36, 152-157. observations were made on 2013 October 25-26, 28-31. The telescope was a 0.50-m Ritchey-Chretien optical tube assembly on Hawkins, S., Ditteon, R. (2008). “Asteroid Lightcurve Analysis at a Paramount ME mount. A Santa Barbara Instrument Group STX- the Oakley Observatory – May 2007.” Minor Planet Bulletin 35, 1- 16803 CCD camera, binned 3x3, with a luminance filter was used 4. in conjunction with the telescope to collect raw images. Images were taken at exposure times of 90, 120, and 150 seconds. The Warner, B. (2006). “Asteroid Lightcurve Analysis at the Palmer image scale was 1.34 arcseconds per pixel (binned) at f/8.3. Raw Divide Observatory – March-June 2006” Minor Planet Bulletin 33, images were processed in CCDSoft using screen flats, bias, and 85-88. dark frames. MPO Canopus was used the measure the processed images and produce lightcurves. In order to maximize the potential for data collection, target asteroids were selected based upon their position in the sky approximately 1 hour after sunset. Higher priority was given to asteroids with previously unknown periods. Objects with uncertain periods were also measured to improve upon previous results.

Lightcurves were produced for 1384 Kniertje, 2161 Grissom, 3062 Wren, and (22412) 1995 UQ4. However, the other three lacked sufficient data to do so. For these asteroids, only magnitude variations are reported. Two of the lightcurves produced were for asteroids for which there were no previous published findings. The other two lightcurves already had published periods: 1348 Kniertje and 3062 Wren. Comments on these publications are included below.

1384 Kniertje: The rotational period found is within 1% of the 9.8071 h period reported in Behrend (2007); however, it does not lie within the reported range of uncertainty, ± 0.0024 h. Similarly, the period found is very close to 9.824 h, the value reported in Hawkins and Ditteon (2008), but does not lie within the ± 0.001 h uncertainty. Warner (2006) found a possible fit at 9.816 h, but ultimately found and reported a better fit: 12.255 ± 0.004 h. A fit

Data Period P. E. Amp A. E. Number Name Dates(MM/DD/2013) Points (h) (h) (mag) (mag) 1359 Prieska 10/25-26, 28-31 74 0.05 0.04 1384 Kniertje 10/25-26, 28, 30 72 9.872 0.012 0.35 0.03 2161 Grissom 10/25-26, 28-31 109 5.0633 0.0012 0.31 0.02 3062 Wren 10/25-26, 29-31 103 7.097 0.003 0.26 0.02 6043 Aurochs 10/25-26, 28-31 79 0.45 0.05 22412 1995 UQ4 10/25-26, 28-31 88 4.487 0.001 0.27 0.03 24393 2000 AG183 10/25-26, 28, 30-31 80 0.40 0.05 Table I. Observing circumstances and results. Minor Planet Bulletin 41 (2014) 170 ROTATIONAL PERIOD OF 2770 TSVET

Lorenzo Franco Balzaretto Observatory (A81), Rome, ITALY [email protected]

Riccardo Papini Carpione Observatory (K49), Spedaletto, Florence, ITALY

(Received: 10 April)

Photometric observations of main-belt asteroid 2770 Tsvet were made over three nights during 2014 March. Lightcurve analysis shows a synodic period P = 7.82 ± 0.01 h with an amplitude A = 0.47 ± 0.03 mag.

The main-belt asteroid 2770 Tsvet was selected from the “Potential Lightcurve Targets” web site (Warner, 2014). Observations on three nights during 2014 March were carried out from Balzaretto Observatory (A81) in Rome (Italy) using a 0.20-m Schmidt- Cassegrain (SCT), reduced to f/5.5, equipped with a SBIG ST7- XME CCD camera, and from Carpione Observatory (K49), near Florence (Italy), using a 0.25-m f/10 Schmidt-Cassegrain (SCT) and SBIG ST9-XE CCD camera. Differential photometry and period analysis were done using MPO Canopus (Warner, 2013). All unfiltered images were calibrated with dark and flat-field frames and the asteroid magnitude was reduced to R band, using near-solar color index compare stars, selected via the Comp Star Selector feature in MPO Canopus.

The derived synodic period was P = 7.82 ± 0.01 h (Fig.1) with an amplitude of A = 0.47 ± 0.03 mag.

Figure 1.The lightcurve of 2770 Tsvet with a period of 7.82 ± 0.01 h and an amplitude of 0.47 ± 0.03 mag.

References

Warner, B.D. (2013). MPO Software, Canopus version 10.4.3.17. Bdw Publishing. http://minorplanetobserver.com/

Warner, B.D. (2014). “Potential Lightcurve Targets.” http://www.MinorPlanet.info/PHP/call_OppLCDBQuery.php

Minor Planet Bulletin 41 (2014) 171

ASTEROIDS OBSERVED FROM CS3: periods reported by Binzel (1987), Slivan (1996) and Behrend 2014 JANUARY - MARCH (2007). This result is in good agreement with those rotational periods. Durech (2011) did a shape model deriving two possible Robert D. Stephens pole solutions with the preferred one at 176º, 68º. It has a sidereal Center for Solar System Studies (CS3)/MoreData! period of 14.07691 h. He used four cords obtained from an 11355 Mount Johnson Ct., Rancho Cucamonga, CA 91737 USA occultation on 2003 December 31 to refine the model, but could not clearly reject either possible pole solution. This synodic result (Received: 1 April) is consistent with that period and might help rule out one of the possible pole positions.

CCD photometric observations of 15 asteroids were 317 Roxane. Roxane has rotational periods reported by Lagerkvist obtained from the Center for Solar System Studies from (1982), Harris (1992), and by Behrend (2013) in 2005, 2007, and 2014 January to March. 2009. All of these periods are similar to the one reported here.

502 Sigune. Sigune has had its rotational period measured many The Center for Solar System Studies (CS3, MPC U81) normally times over the years, all with similar results. Tedesco (1979) first focuses on families of asteroids for its program studies. These observed in reporting a period of 10.5 h. The author (Stephens targets are usually dim, so ‘Full Moon Projects’ are undertaken 2007) observed it over nine nights in June 2007 finding a period of when the moon is bright or close to the targets. These Full Moon 10.922 h. Behrend (2013) reports lightcurves from 2010 and 2011. Projects are often selected from the ‘Shape/Spin Modeling Opportunities’ list maintained by Josef Ďurech the back of each 616 Elly. This Main Belt asteroid has had its rotational period Minor Planet Bulletin. These are targets with at least one high determine three times in the past. Alverez (2004), Durkee (2010), quality lightcurve which are not in the Database of Asteroid and Warner (2010) all reported periods with 0.03 h of this result. Models from Inversion Techniques (DAMIT). In addition, bright NEOs or Mars Crossers away from the Moon will be selected. 670 Ottegebe. Lightcurves of Ottegebe have been obtained several times in recent years. Kirkpatrick (2003) and Buchheim (2007) All images were made with a 0.4-m or 0.35-m SCT with a FLI- measured the rotational period to be about 10.04 h while Chiorny 1001e or a SBIG STL-1001E CCD camera. Images were unbinned (2007) found it to be 10.375 h. This result is closer to the with no filter and had Master flats and darks applied to the science Kirkpatrick and Buchheim period. frames prior to measurement. Measurements were made using MPO Canopus, which employs differential aperture photometry to 822 Lalage. This Main-Belt asteroid has had its rotational period produce the raw data. Period analysis was done using MPO determined twice before. Wisniewski (1997) and Higgins (2011) Canopus, which incorporates the Fourier analysis algorithm both found its period to be with 0.001 h of this result. (FALC) developed by Harris (1989). Night-to-night calibration of the data (generally < ±0.05 mag) was done using field stars 855 Newcombia. Cooney et al (2007) determined that converted to approximate Cousins V magnitudes based on 2MASS Newcombia’s rotational was 3.003 h, virtually identical to this J-K colors (Warner 2007). The Comp Star Selector feature in MPO result. Canopus was used to limit the comparison stars to near solar color. 1219 Britta. Britta’s rotational period is well determined. Pilcher 155 Scylla. Scylla’s rotational period has been determined many (1985), Binzel (1987), Behrend (2013), and Kryszczynska (2012) times over the years. Students at Rose-Hulman (Addleman et al all report periods within 0.001 h of this result. 2005) observed it on three nights in March – April 2005 determining a period of 7.958 h. Pilcher (2009) observed it on 1294 Antwerpia. This Main-Belt asteroid had its rotational period seven nights in 2008 November – December determining a period measured three times. Almeida (2004), LeCrone (2005), and of 7.97597 h. At the same time, Owings (2009) observed it on five Behrend (2013) reported a period very close to this result of 6.62 h. nights determining a rotational period of 7.960 h. The synodic rotational found this year is consistent with those results. 1374 Isora. This Mars-crosser was observed by Winsiewski et al (1995) who reported a rotational period of 8 h. The results this year 208 Lacrimosa. This Hungaria Family asteroid has rotational have a best fit of 36.699 h and an amplitude of 0.12 mag.

2014 Number Name mm\dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 155 Scylla 02/12-02/13 320 10.7,10.3 158 14 7.955 0.005 0.16 0.02 208 Lacrimosa 01/14-01/16 576 11.2,10.5 143 2 14.054 0.005 0.29 0.02 317 Roxane 02/17-02/18 351 12.8,13.2 121 -1 8.173 0.002 0.71 0.02 502 Sigune 03/17-03/20 481 24.8,24.3 217 31 10.924 0.003 0.47 0.02 616 Elly 02/12-02/13 294 6.4,6.1 153 9 5.300 0.005 0.40 0.02 670 Ottegebe 02/14-02/15 313 8.3,8.0 170 -1 10.010 0.006 0.35 0.02 822 Lalage 01/14-01/15 418 16.1,15.6 139 -1 3.3460 0.0005 0.67 0.02 855 Newcombia 03/16-03/17 292 12.7,12.2 197 2 3.002 0.001 0.41 0.02 1219 Britta 01/17-01/18 474 7.8,8.4 106 6 5.573 0.001 0.57 0.02 1294 Antwerpia 01/16-01/17 301 12.9,12.6 146 9 6.620 0.005 0.42 0.02 1374 Isora 01/06-01/28 1711 2.6,0.9,9.5 110 1 36.699 0.001 0.12 0.03 2381 Landi 02/17-02/18 307 15.1,15.5 119 -7 3.985 0.001 1.04 0.02 3496 Arieso 01/06-01/10 266 15.5,13.5 112 -18 2.862 0.001 0.30 0.03 52317 1992 BC1 01/11-02/02 1128 11.6,4.3,6.1 125 -7 34.07 0.01 0.11 0.02 55532 2001 WG2 12/11-01/05 834 1.7,1.4,26.4 76 3 46.08 0.08

Minor Planet Bulletin 41 (2014) 172

However, when the amplitude is this low, Harris (2013) has shown Durkee, R. (2010). “Asteroids Observed from the Shed of Science that single modal and trimodal shapes are also possible. As a test Observatory: 2009 October - 2010 March.” Minor Planet Bul. 37, of the solution, the lightcurve was folded upon itself where the 125-127. second extrema is laid upon the first to see how symmetrical the lightcurve is. This test was inconclusive meaning that an alias of a Durech, J., Kaasalainen, M., Herald, D., Dunham, D., Timerson, half period could exist. B., Hanus, J., F., Frappa, E., Talbot, J., Hayamizu, T., Warner, B. D., Pilcher, F., Galád, A. (2011). “Combining asteroid models 2381 Landi. Almeida (2004) observed Landi in 2000 reporting a derived by lightcurve inversion with asteroidal occultation rotational period of 3.91 h. This result of 3.985 h is in good silhouettes.” Icarus 214, 652-670. agreement with that result. Harris, A.W. (2013). “On the maximum amplitude of harmonics of 3496 Arieso. There are no previously reported rotational periods an asteroid lightcurve.” The Society for Astronomical Sciences 31st for this Mars Crosser in the Lightcurve Database (Warner 2013). Annual Symposium. 2012., 59-63.

(52317) 1992 BC1. This Phocaea family asteroid does not have a Harris, A.W., Young, J.W., Dockweiler, T., Gibson, J., Poutanen, previously reported rotational period. Because of its low M., Bowell, E. (1992). “Asteroid lightcurve observations from amplitude, single modal and trimodal shapes are also possible. As 1981.” Icarus 95, 115-147. a test, the lightcurve was folded upon itself which revealed a slight asymmetry between the two halves. The 34.07 h is our preferred Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., period. Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, (55532) 2001 WG2. There are no previously reported periods for 24, 60, 261, and 863.” Icarus 77, 171-186. this Apollo asteroid in the Lightcurve Database (Warner 2013). After three weeks of observations, a satisfactory period could not Higgins, D. (2011) “Period Determination of Asteroid Targets be derived and the object appeared to be tumbling. Petr Parvec Observed at Hunters Hill Observatory: May 2009 - September (private communication) confirmed that the asteroid is tumbling, 2010.” Minor Planet Bul. 38, 41-46. but from the data obtained, a unique two-period solution could not be obtained. The lightcurve plot is phased to what appears to be the Kirkpatrick, E., Hirsch, B., Lecrone, C., Schwoenk, D., Shiery, M., primary period. Tollefson, E., Twarek, A., White, S., Wolfe, C. (2003). “Oakley Observatory lightcurves of asteroids 670 Ottegebe and 1035 References Amata.” Minor Planet Bul. 30, 41.

Addleman, D., Covele, B., Duncan, A., Johnson, K., Kramb, S., Kryszczynska, A., Colas, F., Polinska, M., Hirsch, R., Ivanova, V., Lecrone, C., Reichert, C., Starnes, H., Twarek, A., Kirkpatrick, E., Apostolovska, G., Bilkina, B., Velichko, F.P., Kwiatkowski, T., Ditteon, R. (2005). “Rose-Hulman spring 2005 lightcurve results: Kankiewicz, P., Vachier, F., Umlenski, V., Michalowski, T., 155 Scylla, 590 Tomyris, 1655 Comas Solá, 2058 Roka, 6379 Marciniak, A., Maury, A., Kaminski, K., Fagas, M., Dimitrov, W., Vrba, and (25934) 2001 DC74.” Minor Planet Bul. 32, 76-48. Borczyk, W., Sobkowiak, K., Lecacheux, J., Behrend, R., Klotz, A., Bernasconi, L., Crippa, R., Manzini, F., Poncy, R., Antonini, Alvarez-Candal, A., Duffard, R., Angeli, C., Lazzaro, D., P., Oszkiewicz, D., Santana-Ros, T. (2012). “Do Slivan states exist Fernández, S. (2004). “Rotational lightcurves of asteroids in the Flora family?. I. Photometric survey of the Flora region.” belonging to families.” Icarus 172, 388-401. Astronomy & Astrophysics, 546, 51.

Behrend, R., (2013). Observatoire de Geneve web site, Lagerkvist, C.-I., Rickman, H. (1982). “On the Rotation of M http://obswww.unige.ch/~behrend/page_cou.html Asteroids.” Sun and Planetary System 96, 289.

Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.” Almeida, R., Angeli, C. A., Duffard, R., Lazzaro, D. (2004). Icarus 72, 135-208. “Rotation periods for small main-belt asteroids.” Astronomy and Astrophysics, 415, 403-406. Binzel, R.P., Cochran, A.L., Barker, E.S., Tholen, D.J., Barucci, A., di Martino, M., Greenberg, R., Weidenschilling, S.J., Owings, L. (2009). “Lightcurves for 155 Scylla and 2358 Bahner.” Chapman, C.R., Davis, D.R. (1987). “Coordinated observations of Minor Planet Bul. 36, 51-52. asteroids 1219 Britta and 1972 Yi Xing.” Icarus 71, 148-158. Pilcher, F., Binzel, R., Tholen, D. (1985). “Rotations of 1168 Buchheim, R. (2007). “Lightcurves for 122 Gerda, 217 Eudora, Brandia and 1219 Britta.” Minor Planet Bul. 12, 10. 631 Phillipina 670 Ottegebe, and 972 Cohnia.” Minor Planet Bul. 34, 13-14. Pilcher, F., Jardine, D. (2009). “Period Determinations for 31 Euphrosyne, 35 Leukothea 56 Melete, 137 Meliboea, 155 Scylla, Chiorny, G., Shevchenko, V., Krugly, Y., Velichko, F., Gaftonyuk, and 264 Libussa.” Minor Planet Bul. 36, 52-54. N. (2007). “Photometry of asteroids: Lightcurves of 24 asteroids obtained in 1993 – 2005.” Planetary and Space Science, 55, 986- Slivan, S., Binzel, R. (1996). “Forty-eight New Rotation 997. Lightcurves of 12 Koronis Family Asteroids.” Icarus 124, 452- 470. Cooney, W., Jr., Gross, J., Terrell, D., Reddy, V., Dyvig, R. (2007). “Lightcurve Results for 486 Cremona, 855 Newcombia Stephens, R. (2007). “Photometry from GMARS and Santana 942 Romilda, 3908 Nyx, 5139 Rumoi, 5653 Camarillo, (102866) Observatories - April to June 2007.” Minor Planet Bul. 34, 102- 1999 WA5.” Minor Planet Bul. 34, 47-49. 103.

Minor Planet Bulletin 41 (2014) 173 Tedesco, E. (1979). PhD Dissertatin, New Mex. State Univ. 280.

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

Warner, B.D. (2010). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2009 December - 2010 March.” Minor Planet Bul. 37, 112-118.

Warner, B.D. (2013). The Asteroid Lightcurve Database (LCDB) website. http://www.minorplanet.info/lightcurvedatabase.html.

Wisniewski, W., Michalowski, T., Harris, A., McMillan, R. (1995), “Photoelectric Observations of 125 Asteroids.” Abstracts of the Lunar and Planetary Science Conference, 26, 1511.

Acknowledgements

This research was supported by National Science Foundation grant AST-1212115 and by NASA grant NNX13AP56G.

The purchase of the FLI-1001E CCD camera was made possible by a 2013 Gene Shoemaker NEO Grant from the Planetary Society.

Minor Planet Bulletin 41 (2014) 174

Minor Planet Bulletin 41 (2014) 175

ROTATIONAL PERIOD, HR-G PARAMETERS, COLOR INDEX, AND DIAMETER ESTIMATION FOR 473 NOLLI

Eduardo Manuel Álvarez OLASU (I38) Costanera Sur 559, Salto 50.000, URUGUAY [email protected]

Frederick Pilcher Organ Mesa Observatory (G50) 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA

(Received: 11 April)

Photometric measurements for asteroid 473 Nolli were performed from two observatories during its 2014 favorable opposition. The synodic rotation period was found to be 3.0785 ± 0.0001 h, the lightcurve amplitude was 0.19 ± 0.02 mag, the absolute R-band magnitude was 11.500 ± 0.029 mag, the slope parameter was 0.253 ± 0.047, and the V-R color index was 0.453 ± 0.034 mag. These led to an estimated diameter of 13 ± 3 km.

473 Nolli is a main-belt asteroid discovered in 1901 by M. Wolf at Heidelberg (Germany). It appeared on the CALL web site as an asteroid photometry opportunity due to it reaching a favorable apparition in 2014 and having no defined lightcurve parameters.

Observations by Álvarez were made at Observatorio Los Algarrobos, Salto, Uruguay (OLASU, MPC Code I38) in 2014 from February 8 to April 9, with a 0.30-m Meade LX-200R telescope and QSI 516wsg CCD, guided, 2x2 binning, clear, V and R filter, and 120 to 150 second exposures. Observations by Pilcher were made at the Organ Mesa Observatory (MPC code G50) in 2014 from January 29 to February 19, with a 0.35-m Meade LX200 GPS telescope and SBIG STL-1001E CCD, unguided, clear filter, and 60-second exposures.

Our computers were synchronized with atomic clock time via Internet NTP servers at the beginning of each session. All images were dark and flat-field corrected and then measured using MPO Canopus software (Bdw Publishing) version 10.4.3.16 with a differential photometry technique. The data were light-time corrected. Night-to-night zero point calibration was accomplished by selecting up to five comp stars with near solar colors according to recommendations by Warner (2007) and Stephens (2008). Period analysis was also done with MPO Canopus, which

incorporates the Fourier analysis algorithm developed by Harris (Harris et al., 1989).

Almost 50 hours of effective observation and more than 1,200 data points were required in order to solve the lightcurve (Figure 1). Over the 70-day span of observations, the phase angle varied from –14.29º to –1.31º and from +1.26 º to +16.97º, the phase angle bisector ecliptic longitude from 159.1º to 162.0º, and the phase angle bisector ecliptic latitude from 0.0º to –5.1º. The rotation period for 473 Nolli was determined to be 3.0785 ± 0.0001 h along with a peak-to-peak amplitude of 0.19 ± 0.02 mag. The lightcurve showed a typical bimodal shape, with the maxima virtually identical in magnitude, and the minima differing by only a small – although noticeable – amount. In spite of its short (potentially favorable) period no evidence of binary companion was seen in the lightcurve.

Minor Planet Bulletin 41 (2014) 176

The absolute R-band magnitude (HR) and slope parameter (G) were Lagerkvist, C.I., Magnusson, P. (1990). “Analysis of Asteroid found using the H-G Calculator tool of MPO Canopus, which is Lightcurves. II. Phase curves in a generalized HG system.” Astron based on the FAZ algorithm developed by Alan Harris (1989). Six & Astrophys Suppl. Series 86, 119. pre- and five post-opposition data were used (Figure 2), all of them representing the maximum of the curve for each observing session. Minor Planet Center asteroid catalog MPCORB Web Site. The absolute R-band magnitude was determined to be 11.500 ± http://www.minorplanetcenter.org/iau/MPCORB.html 0.029 mag and the slope parameter 0.253 ± 0.047, typical of intermediate albedo asteroids (Lagerkvist and Magnusson, 1990). Pravec, P., Harris, A.W. (2007). “Binary Asteroid Population I. Angular Momentum Content.” Icarus 158, 106-145. The color index was found to be V-R = 0.453 ± 0.034 mag (mean of 34 values found from the session of March 8). By adding the Pravec, P., Harris, A.W., Kusnirák, P., Galád, A. Hornoch, K. (2012). “Absolute Magnitudes of Asteroids and a Revision of mean V-R color index to the HR value, we obtained an absolute visual magnitude H = 11.953 ± 0.063 mag. In agreement with the Asteroid Albedo Estimates from WISE Thermal Observations.” systematic offset of H catalog values for small asteroids recently Icarus 221, 365-387. reported by Pravec et al. (2012), our H value is slightly larger than those published at the JPL Small-Body Database (H = 11.6 mag) Shevchenko, V.G., Lupishko, D.F. (1998). “Optical Properties of and at the Minor Planet Center’s MPCORB catalog (H = 11.7 Asteroids from Photometric Data.” Solar System Research 32, 220- mag). 232.

According to Shevchenko and Lupishko (1998), our measured Stephens, R.D. (2008). “Long Period Asteroids Observed from V-R color index is halfway between those corresponding for GMARS and Santana Observatories.” Minor Planet Bul. 35, 21-22. taxonomical types S (0.49 mag) and M (0.42 mag). For those basic Warner, B.D. (2007). “Initial Results from a Dedicated H-G compositional types of asteroids, the geometric albedo on the Project.” Minor Planet Bul. 34, 113-119. Johnson V band (pV) respectively are 0.20 and 0.17. By assuming an intermediate pV = 0.185, the formula by Pravec and Harris (2007) for the asteroid diameter (D) in kilometers

gives an estimated diameter of D = 13 ± 3 km.

Our study now leaves only three asteroids numbered below 500 for which no rotation parameters are currently found in the literature. They are 299 Thora, 398 Admete, and 457 Alleghenia. Among the asteroids numbered from 501 to 1000, 23 still have no period that we could find. This is a dramatic reduction from two years ago (Alvarez, 2012), thus leaving only 26 among the first 1000 Figure 1. Composite lightcurve of 473 Nolli. numbered asteroids with no previously reported rotation period. However, even in cases where low numbered asteroids do have reported lightcurve parameters, not all of these period determinations are secure (i.e., many have U < 3) and ongoing investigations to verify, refine, or revise their values remains an important and pending endeavor.

References

Alvarez, E.M. (2012). “Period Determination for 414 Liriope.” Minor Planet Bul. 39, 21-22.

Collaborative Asteroid Lightcurve Link (CALL) Web Site. http://www.minorplanet.info/PHP/call_OppLCDBQuery.php

Harris, A.W. (1989). “The H-G Asteroid Magnitude System: Mean Slope Parameters.” Abstracts of the Lunar and Planetary Science Conference 20, 375. Figure 2. H-G plot in R-band magnitude for 473 Nolli. 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, 24, 60, 261, and 863.” Icarus 77, 171-186.

Jet Propulsion Laboratory Small-Body Database Browser Web Site at http://ssd.jpl.nasa.gov/sbdb.cgi#top

Minor Planet Bulletin 41 (2014) 177

ASTEROID LIGHTCURVE ANALYSIS AT 0.65 ± 0.02 mag, suggesting that the asteroid rotated 31 times RIVERLAND DINGO OBSERVATORY (RDO) during the period of observation.

Kevin Hills (98889) 2001 BL38 is a Mars-crossing asteroid discovered by Riverland Dingo Observatory LINEAR at Socorro in 2001. A total of 1,883 data points were Moorook 5343, South Australia obtained over seven nights during the period 2014 March 12 –30 AUSTRALIA as the solar phase angle increased from +23.3° to +26.2°. The [email protected] average magnitude was 15.7 and average SNR was 23. The lightcurve shows a period of 5.421 h ± 0.001 h and amplitude of (Received: 13 April) 0.27 ± 0.05 mag, suggesting that the asteroid rotated 80 times during the period of observation.

Lightcurves for five asteroids selected from the Acknowledgements Collaborative Asteroid Lightcurve Link (CALL) were obtained at RDO in the period 2013 September 15 – The measurements reported make use of the AAVSO Photometric 2014 March 30: 3992 Wagner, 4511 Rembrandt, (6652) All-Sky Survey (APASS) catalog, which is funded by the Robert 1991 SJ1, (16009) 1999 CM8, and (98889) 2001 BL38. Martin Ayers Sciences Fund.

Thank you to Darren Wallace of RDO and his collaborators at The observations reported here were all obtained using a 0.41-m New Mexico Skies for maintaining the equipment in Australia. f/9 Ritchey-Chretien telescope and SBIG STL-1001E CCD camera with a Johnson-Cousins V filter. All images were bias, dark, and flat field corrected and had an image scale of 1.35 arc seconds per pixel.

Differential photometry measurements were made in MPO Canopus (Bdw Publishing). V magnitudes for comparison stars were extracted from the AAVSO Photometric All-Sky Survey (APASS) catalog.

The Asteroid Lightcurve Database (LCDB) does not contain any previously reported results for any of the asteroids reported here.

3992 Wagner is a main-belt asteroid discovered by F. Borngen at Tautenburg in 1987. A total of 962 data points were obtained over 14 nights during the period 2013 October 1 – November 3 as the solar phase angle increased from +5.9° to +16.3°. The average magnitude was 16.0 and average SNR was 37. The lightcurve shows a period of 20.628 ± 0.004 h and amplitude of 0.29 ± 0.03 mag, suggesting that the asteroid rotated 38 times during the period of observation.

4511 Rembrandt is a main-belt asteroid discovered by H. van Gent at Johannesburg in 1935. A total of 819 data points were obtained over five nights during the period 2013 September 15 – 28 as the solar phase angle increased from +3.8° to +8.9°. The average magnitude was 14.2 and average SNR was 76. The lightcurve shows a period of 3.8369 h ± 0.0002 h and amplitude of 0.49 ± 0.02 mag, suggesting that the asteroid rotated 82 times during the period of observation.

(6652) 1991 SJ1 is a main-belt asteroid discovered by Holt, H. E. at Palomar in 1991. A total of 2,134 data points were obtained over 38 nights during the period 2013 November 24 – 2014 March 8 including solar phase angles between –12.6° to +27.0° (minimum observed +10.6°). The average magnitude was 16.3 and average SNR was 44. The lightcurve shows a period of 85.56 h ± 0.01 h and amplitude of 0.75 ± 0.03 mag, suggesting that the asteroid rotated 29 times during the period of observation.

(16009) 1999 CM8 is a main-belt asteroid discovered by T. Kobayashi at Oizumi in 1999. A total of 577 data points were obtained over 11 nights during the period 2013 November 1 – 23 as the solar phase angle increased from +5.5° to +16.0°. The average magnitude was 15.0 and average SNR was 72. The lightcurve shows a period of 16.70 h ± 0.01 h and amplitude of

Minor Planet Bulletin 41 (2014) 178

References

AAVSO Photometric All-Sky Survey (APASS) catalog. http://www.aavso.org/download-apass-data

Warner, B.D. (2006). Practical Guide to Lightcurve Photometry and Analysis. Springer, New York, NY.

Warner, B.D. (2008). MPO Software, MPO Canopus version 10, Bdw Publishing, Eaton, CO.

Warner, B.D. (2011). Collaborative Asteroid Lightcurve Link website. http://www.minorplanet.info/call.html

ASTEROID PHOTOMETRY FROM with the refractors. All images were unfiltered and were reduced THE PRESTON GOTT OBSERVATORY with dark frames and sky flats.

Dr. Maurice Clark Image analysis was accomplished using differential aperture Department of Physics photometry with MPO Canopus. Period analysis was also done in Texas Tech University MPO Canopus, which implements the algorithm developed by Lubbock TX 79409 Alan Harris (Harris et al., 1989). Differential magnitudes were [email protected] calculated using reference stars from the USNO-A 2.0 catalog and the UCAC3 catalog. (Received: 3 April) Results are summarized in the table below, and the lightcurve plots are presented at the end of the paper. The data and curves are Asteroid period and amplitude results obtained at the presented without additional comment except were circumstances Preston Gott Observatory during the second half of 2013 warrant. Column 3 gives the range of dates of observations and are presented. column 4 gives the number of nights on which observations were undertaken.

The Preston Gott Observatory is the main astronomical facility of 8958 Stargazer. Observations of this asteroid were made on 10 the Texas Tech University. Located about 20 km north of nights, with the period derived being 12.886 hours. The Lubbock, the main instrument is a 0.5-m f/6.8 Dall-Kirkam observations indicated that the two minima were very unequal cassegrain. An SBIG STL-1001E CCD was used with this although the maxima were similar. telescope. Other telescopes used were 0.35-m and 0.30-m Schmidt- Cassegrains (SCT), and 0.13-m refractors. SBIG ST9XE CCD’s (14255) 2000 AS70. This asteroid was observed on four nights. were used with the SCTs and SBIG ST10XE CCD’s were used The derived lightcurve indicated a period of a little under 13 hours, but was quite peculiar in that the second maximum was Minor Planet Bulletin 41 (2014) 179

# Name Date Range Sessions Per (h) Error (h) Amplitude Error 5380 Sprigg Oct 13 – Oct 27, 2013 3 3.219 0.002 0.68 0.02 5450 Sokrates Dec 11, 2013 – Jan 3, 2014 4 5.9822 0.0003 0.37 0.01 5707 Shevchenko Dec 11, 2013 – Jan 3, 2014 4 3.0081 0.0001 0.46 0.01 6516 Gruss Sept 29 – Nov 29, 2013 5 13.003 0.008 0.09 0.05 7454 Kevinrighter Oct 17, 2013 1 4.014 0.001 0.59 0.05 8866 Tanegashima Dec 11, 2013 – Jan 3, 2014 4 13.525 0.003 0.48 0.03 8958 Stargazer Nov 10 – Dec 11, 2013 3 15.991 0.002 0.62 0.05 10465 1980 WE5 Oct 27 – Dec 11, 2013 5 7.4403 0.0005 0.48 0.1 11958 Galiani Dec 31, 2013 – Jan 12, 2014 3 9.8013 0.0023 0.96 0.05 12920 1998 VM15 Aug 9 – Nov 10, 2013 9 12.885 0.001 0.31 0.05 13026 1989 CX Dec 31, 2013 – Jan 12, 2014 4 6.163 0.002 0.36 0.1 14255 2000 AS70 Dec 11, 2013 – Jan 3, 2014 4 12.772 0.002 0.32 0.05 16135 Ivarsson Nov 29, 2013 – Jan 3, 2014 5 8.273 0.003 0.31 0.1 19682 1999 RW194 Dec 31, 2013 – Jan 3, 2014 3 2.5353 0.0008 0.21 0.1 20561 1999 RE120 Jan 3 – Jan 12, 2014 2 4.550 0.001 0.61 0.1 20744 2000 AO151 Sept 29, 2013 – Jan 3, 2014 7 28.64 0.01 0.29 0.1 21107 1992 PZ4 Aug 9 – Sept 8, 2013 4 3.289 0.001 0.13 0.1 26022 4180 P-L Nov 29, 2013 1 5.402 0.001 0.91 0.2 28461 2000 AL164 Oct 6 – Oct 13, 2014 2 3.440 0.002 0.09 0.5 34726 2001 QA25 Oct 27, 2013 – Jan 3, 2014 6 15.47 0.01 0.61 0.1 36439 2000 PT26 Nov 29, 2013 – Jan 1, 2014 4 5.5786 0.0002 0.50 0.5 85118 1971 UU Aug 9 – Sept 29, 2013 4 10.098 0.001 1.12 0.02 87073 2000 KF66 Sept 29 – Nov 3, 2013 5 10.972 0.002 0.20 0.1 113781 2002 TF188 Oct 13, 2013 1 1.978 0.101 0.75 0.1 120279 2004 HE18 Nov 29, 2013 1 3.89 0.11 1.08 0.1 306695 2000 VL1 Dec 31, 2013 – Jan 12, 2014 4 9.930 0.002 0.76 0.05 326317 1999 VN23 Nov 3 – Nov 10, 2013 2 2.98 0.01 0.18 0.05

substantially smaller than the first. However, since the period was close to half a day, this second maximum was poorly observed.

(16141) 1999 XT147. This asteroid was observed on one night when it was in the field of another asteroid being studied. Despite having only one night of data, a complete lightcurve was obtained.

(85118) 1971 UU. Observations of this asteroid were made on four nights. Although the complete lightcurve was not observed, sufficient data were obtained to derive a period of 10.098 h with a large amplitude of 1.12 mag. The two maxima were unequal.

(113781) 2002 TF188. This asteroid was observed on one night when it was in the field of another asteroid. Unfortunately the full period was not covered. A single-maximum period of 1.978 hours was derived, but an attempt to derive a more normal 2-maxima period was not successful due to insufficient data. From the data obtained, a full period of just under 4 hours is probably the true one, however more observations are required to confirm this. (120279) 2004 HE18. This asteroid was observed on one night when it was in the field of another asteroid. The asteroid was quite faint and so the data were very noisy; however, a period of 3.89 hours was derived. More observations are required to confirm this.

(326317) 1999 VN23. This asteroid was observed on two nights. The derived lightcurve was quite asymmetric, with the two maxima being unequal. More observations would be useful to confirm this.

Acknowledgments

I would like to thank Brian Warner for all of his work with the program MPO Canopus and for his efforts in maintaining the “CALL” website.

References

Warner, B.D. (2011). Collaborative Asteroid Lightcurve Link website. http://www.minorplanet.info/call.html Minor Planet Bulletin 41 (2014) 180

Minor Planet Bulletin 41 (2014) 181

Minor Planet Bulletin 41 (2014) 182

Minor Planet Bulletin 41 (2014) 183

Minor Planet Bulletin 41 (2014) 184

PERIOD DETERMINATION OF 1246 Chaka. This target required ten sessions over a span of almost SIX MAIN BELT ASTEROIDS five months because of bad weather. A little portion of the curve was not covered with observations, but the final lightcurve is well- Andrea Ferrero determined, with a period of 25.44 ± 0.01 h and amplitude A = Bigmuskie Observatory 0.25 mag. via Italo Aresca 12 14047 Mombercelli, Asti, ITALY 2834 Christy Carol. Despite this target showing a period P = 12.79 ± 0.01 h with an amplitude A = 0.39 mag, very close to half of an (Received: 14 April) Earth day, it was possible to cover the entire curve with six sessions spaced over a period of about a month.

Observations of six main-belt asteroids (MBA) produced Acknowledgments lightcurve parameters of: 487 Venetia, P = 13.34 ± 0.01 h, A = 0.20 mag; 684 Hildburg, P = 15.89 ± 0.01 h, A = Thanks to Lorenzo Franco of the Balzaretto Observatory for his 0.22 mag; 772 Tanete, P = 8.629 ± help on 1181 Lilith. 0.001 h, A = 0.18 mag.; 1181 Lilith, P = 15.04 ± 0.01 h, A = 0.11 mag.; 1246 Chaka, P = 25.44 ± 0.01 h, A = References 0.25 mag.; and 2834 Christy Carol, P = 12.79 ± 0.01 h, A = 0.39 mag. Warner, B.D. (2012). MPO Software, MPO Canopus v10.4.1.9. Bdw Publishing, Eaton, CO.

Starting from late 2013 till 2014 April, six main-belt asteroids were observed at the Bigmuskie Observatory. For one of them, 684 Hildburg, it was impossible to distinguish between two periods, one of which is almost exactly half an Earth day.

The standard setup for the observations is a Marcon 0.30-m f/8 Ritchey-Chretién telescope coupled to an SBIG ST-9 CCD camera with a pixel array of 512x512x20 microns. Images were taken using an Astrodon R filter. MPO Canopus v10.4.1.9 (Warner, 2012) was used for image calibration and photometric measurements. Night-to-night zero-point calibration was done using the Comparison Star Selector utility in MPO Canopus and from three to five solar-colored comparison stars from the APASS catalog. This combination produces, in good sky conditions, a very precise linkage between the sessions, in the range of ± 0.03, or even 0.02 mag. Only in case of foggy nights or in presence of the moon, do these values increase by a factor to two or three times.

487 Venetia. For this target, it was possible to reach a secure result with four sessions. A period of 13.34 ± 0.01 h and amplitude 0.20 mag leaves no room for other possibilities.

684 Hildburg. This target shows two different periods, both with good chance to be correct. The first is P = 15.89 ± 0.01 h and amplitude A = 0.22 mag, while the second, almost equal to half the earth rotation, is P = 11.92 ± 0.01 h and amplitude A = 0.21 mag. MPO Canopus has a slight preference for the longer period, evident from the period spectrum, but the difference is so tiny that it is not sure which period is right.

772 Tanete. Because of the location of the observatory, it was possible to work on this target only in the second part of the night with fairly short sessions of three or four hours in the beginning and five hours at the end. Because of this, the period of 8.629 ± 0.001 h with an amplitude A = 0.18 mag was found only after ten sessions. The lightcurve is an unusual monomodal curve.

1181 Lilith. Even if the period shows no alias, the strange attenuation at phase 0.90-1.00 is very interesting. It seems to be the evidence of a second asteroid orbiting around 1181 Lilith. After a specific investigation to find the smaller component, worked together with Lorenzo Franco of Balzaretto Observatory, it seems that the bump is only scattering in the data. Unfortunately the target became too faint to go on with observations to erase any doubts. The final period is 15.04 ± 0.01 h with an amplitude A = 0.11 mag. Minor Planet Bulletin 41 (2014) 185

Minor Planet Bulletin 41 (2014) 186

ASTEROID LIGHTCURVE ANALYSIS AT ELEPHANT Fauerbach, M., Bennett, T. (2005). “Photometric lightcurve HEAD OBSERVATORY: 2013 OCTOBER-NOVEMBER observations of 125 Liberatrix, 218 Bianca, 423 Diotima, 702 Alauda, 1963 Bezovec, and (5849) 1990 HF1.” Minor Planet Bul. Michael S. Alkema 32, 80-81 Elephant Head Observatory (G35) Sahuarita, AZ 85629 Florczak, M., Dotto, E., Barucci, M.A., Birlan, M., Erikson, A., [email protected] Fulchignoni, M., Nathues, A., Perret, L., Thebault, P. (1997). “Rotational properties of main belt asteroids: photoelectric and (Received: 15 April) CCD observations of 15 objects.” Planet. Space Sci. 45, 1423- 1435.

Photometric observations of three main-belt asteroids Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., were obtained at Elephant Head Observatory during Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, 2013 October to December: 702 Alauda, 1246 Chaka, H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids and 4067 Mikhelson. 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid The synodic rotation rates for three main-belt asteroids were Lightcurve Database.” Icarus 202, 134-146. Updates at: determined from the analysis of CCD photometric observations. http://www.minorplanet.info/lightcurvedatabase.html Observations were conducted with a 0.36-m Schmidt-Cassegrain Telescope on a German Equatorial mount (GEM) using an SBIG STT-8300M CCD camera with 5.4 micron pixels binned at 4x4 with an image scale of 1.56 arcsecond per pixel. A clear filter was used for all exposures. All images were dark and flat-field corrected. All lightcurve data were submitted to the ALCDEF website (http://www.minorplanetcenter.net/light_curve).

All images were obtained from an automated image routine using CCDAutopilot v5. Imaging and plate solving were done with Maxim DL v5 and TheSkyX v10. Data were reduced in MPO Canopus v10 using differential photometry. Comparison stars were chosen for near-solar color index with the “comp star selector” of MPO Canopus. Period analysis was completed using MPO Canopus, which incorporates the Fourier analysis algorithm developed by Harris (FALC; Harris et al., 1989). These asteroids were reported as lightcurve opportunities in the Minor Planet Bulletin.

702 Alauda. A search for previous period determinations of 702 Alauda found Fauerbach and Bennett (2005, 8.348 h) and Benishek (2008, 8.3539 h). New observations were obtained over 8 nights in 2013 Oct. Analysis of the data found a period of 8.3531 ± 0.0004 h, amplitude 0.10 ± 0.01 mag. The newly determined period is in disagreement with that of Fauerbach and Bennett but within experimental uncertainty of Benishek and Protitch- Benishek.

1246 Chaka A search for previous period determinations of 1246 Chaka found Florczak et al. (1997, 20 h). New observations were obtained over 8 nights in 2013 Nov and Dec. Analysis of the data found a period of 18.47 ± 0.01 h, amplitude 0.13 ± 0.02 mag. The newly determined period is in disagreement with that of Florczak et al. Further observations of this asteroid are required to refine the period and amplitude due to the incomplete coverage.

4067 Mikhelson. A search for previous period determinations of 4067 Mikhelson found no published lightcurve period. New observations were obtained over 4 nights in 2013 Oct and Nov. Analysis of the data found a period of 2.2461 ± 0.0004 h, amplitude 0.11 ± 0.02 mag.

References

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

Minor Planet Bulletin 41 (2014) 187

ROTATION PERIOD DETERMINATION filter. Odden and Aggarwal at Phillips Academy Observatory used FOR 163 ERIGONE a 0.4 meter f/8 DFM Engineering telescope and SBIG 1301-E CCD. Frederick Pilcher Organ Mesa Observatory MPO Canopus software was used by all observers to measure the 4438 Organ Mesa Loop images photometrically, share data, adjust instrumental magnitudes Las Cruces, NM 88011 USA up or down to produce the best fit, and prepare the lightcurve. Due [email protected] to the large number of data points acquired the lightcurve has been binned in sets of five data points with a maximum of ten minutes John W. Briggs between points. HUT Observatory P. O. Box 3725 When data for 11 sessions 2014 Feb. 22 - March 29 were Eagle, CO 81631 USA combined they produced a very well defined lightcurve with period 16.136 ± 0.001 hours, amplitude 0.32± 0.02 magnitudes. This is in Luis Martinez complete agreement with Harris and Young (1989). Lenomiya Observatory 515 E. Barrus Place Acknowledgments Casa Grande, AZ 85122 USA Research at the Phillips Academy Observatory is supported by the Caroline Odden and Ashok Aggarwal Israel Family Foundation. Work at HUT Observatory is supported Phillips Academy Observatory by the Michele and David Mittelman Family Foundation. 180 Main Street Andover, MA 01810 USA Reference

(Received: 23 April) Harris, A.W., Young, J.W. (1989). “Asteroid Lightcurve Observations from 1979-1981.” Icarus 81, 314-364.

For 163 Erigone, a rotation period of 16.136 ± 0.001 hours and lightcurve amplitude of 0.32 ± 0.02 magnitude have been found.

The only previous rotation period determination of 163 Erigone is by Harris and Young (1989) who published a period of 16.136 hours.

The several authors all started observing 163 Erigone independently and upon learning of each others work agreed to share their data. Observations by Pilcher were made at the Organ Mesa Observatory with a Meade 35 cm LX200 GPS S-C, SBIG STL-1001E CCD, clear filter, unguided exposures. Briggs made observations at the New Mexico Skies Observatory with a 20 inch PlaneWave f/6.8 corrected Dall-Kirkham telescope operated remotely with ACP software by DC-3 Dreams, and a SBIG STX- 16803 CCD. Martinez at Lenomiya Observatory used a Celestron CPC 1100 28 cm Schmidt Cassegrain, SBIG ST8XME CCD, clear Minor Planet Bulletin 41 (2014) 188

ROTATION PERIOD DETERMINATION FOR 227 PHILOSOPHIA

Frederick Pilcher Organ Mesa Observatory (G50) 4438 Organ Mesa Loop Las Cruces, NM 88011 USA [email protected]

Michael S. Alkema Elephant Head Observatory (G35) 17070 S. Kolb Rd. Sahuarita AZ 85629 USA

(Received: 15 April)

A synodic rotation period of 52.98 ± 0.01 hours, amplitude 0.15 ± 0.02 magnitudes is found for asteroid Figure 1. Period spectrum for 2013 12 27 to 2014 02 22 227 Philosophia. observations of 227 Philosophia.

Previous period determinations for 227 Philosophia are by Bembrick et al. (2006), 18.048 hours; Behrend (2006), 26.138 hours; Alkema (2013), 17.181 hours.

New observations were made in 2013/14 by co-authors Pilcher and Alkema to resolve these ambiguities. Equipment used by Pilcher at the Organ Mesa Observatory include a 35 cm Meade LX200GPS S-C, SBIG STL-1001E CCD, clear filter; and by Alkema at Elephant Head Observatory are a 35 cm S-C, SBIG STT-8300M CCD, clear filter. MPO Canopus software was used for data analysis and data sharing by the two observers.

Observations on 19 nights 2013 Dec. 27 - 2014 Feb. 22 provide a good fit to a lightcurve phased to 52.98 ± 0.01 hours with amplitude 0.15 ± 0.02 magnitudes and complete phase coverage. When phased to the double period of 106.0 hours there is about 95% phase coverage with the two halves of the lightcurve being identical within likely photometric errors. We also provide a Figure 2. Lightcurve for 2013 12 27 to 2014 02 22 observations of period spectrum from 10 to 60 hours, including all previous 227 Philosophia phased to 52.98 hours. reported periods. The only deep minimum other than at 53 hours is for the half period. The 53 hour lightcurve is sufficiently asymmetric that the half period may be safely rejected. All of the previously reported much shorter periods are now definitively ruled out. We consider that the high degree of symmetry in the double period lightcurve makes the double period sufficiently unlikely that we may safely reject it.

We have re-examined the data reported by one of us (Alkema, 2013) for the previous opposition. For the eight sessions 2012 Nov. 25 - 2013 Jan. 12 included in that study we found, after considerable adjustment of the instrumental magnitudes, a good fit to a period of 53.12 ± 0.02 hours and fully compatible with the current study. This is not a completely independent determination because we examined only a fairly small range of periods near 53 hours, and shows only that the earlier data are compatible with a period of 52.98 hours. That a good fit was obtained, however, improves our confidence that the period near 53 hours is the correct one.

Figure 3. Lightcurve for 2012 11 25 to 2013 01 12 observations of 227 Philosophia phased to 53.12 hours.

Minor Planet Bulletin 41 (2014) 189

OBSERVER & OBSERVING NO. References PLANET APERTURE (cm) PERIOD (2012) OBS.

1 Ceres Faure and Rayon, 8 Dec 4 2 Alkema, M. S. (2013). “Asteroid Lightcurve Analysis at Elephant Watson, 20 Jan 2-8 3

Head Observatory 2012 November - 2013 April.” Minor Planet 4 Vesta Watson, 20 Jan 2-8 3

Bull. 40, 133-137. 7 Iris Faure, 8 Aug 17 3

9 Metis Watson, 20 Mar 15-18 3 Behrend, R. (2006). Observatoire de Geneve web site 14 Irene Watson, 20 Mar 18-May 5 3 http://obswww.unige.ch/~behrend/page_cou.html 16 Psyche Pryal, 20 May 6-7 2

Bembrick, C. S., Allen, B., Richards, T. (2006). “Lightcurves from 25 Phocaea Pryal, 20 May 5-6 2 Watson, 20 Aug 6 2 Two Oppositions of 227 Philosophia and 2089 Cetacea.” Minor 83 Beatrix Pryal, 20 May7 6-7 2 Planet Bull. 33, 42-43. 86 Semele Pryal, 20 Oct 13-14 2

89 Julia Pryal, 20 Sep 9-10 2

98 Ianthe Pryal, 20 Jan 17-18 2

GENERAL REPORT OF POSITION OBSERVATIONS 140 Siwa Pryal, 20 May 6-7 2

BY THE ALPO MINOR PLANETS SECTION 156 Xanthippe Pryal, 20 May 5-6 2

FOR THE YEAR 2013 176 Iduna Pryal, 20 Oct 13-14 2 Watson, 20 Sep 28-Oct 3 3

Frederick Pilcher 182 Elsa Pryal, 20 Jan 13-14 2

4438 Organ Mesa Loop 209 Dido Pryal, 20 Oct 26-27 2

Las Cruces, NM 88011 USA 216 Kleopatra Pryal, 20 Dec 11 2

[email protected] 238 Hypatia Pryal, 20 Sep 13 2

324 Bamberga Pryal, 20 Sep 9-10 2

336 Lacadiera Pryal, 20 Jun 4-5 2 Observations of positions of minor planets by members 358 Apollonia Pryal, 20 Oct 26-27 2 of the Minor Planets Section in calendar year 2013 are 378 Holmia Pryal, 20 Oct 26-27 2 summarized. 387 Aquitania Pryal, 20 Jul 7 2 Watson, 20 Jul 12-Aug 6 2

418 Alemannia Pryal, 20 Sep 10 2 During the year 2013 a total of 623 positions of 171 different minor planets were reported by members of the Minor Planets 419 Aurelia Pryal, 20 Sep 13 2

Section. All are approximate visual positions. 435 Ella Pryal, 20 Sep 13 2

451 Patientia Pryal, 20 Jan 13-14 2

The summary lists minor planets in numerical order, the observer 482 Petrina Pryal, 20 Oct 5 2 and telescope aperture (in cm), UT dates of the observations, and 488 Kreusa Pryal, 20 Jan 17-18 2 the total number of observations in that period. The year is 2013 in 511 Davida Pryal, 20 Dec 11 2 each case. 539 Pamina Pryal, 20 Sep 13 2

Positional observations were contributed by the following 568 Cheruskia Pryal, 20 Oct 5 2 observers: 572 Rebekka Pryal, 20 Oct 27 2

587 Hypsipyle Faure and Rayon, 40 Mar 3 3 Observer, Instrument Location Planets Positions 599 Luisa Pryal, 20 Oct 13-14 2 Bookamer, Richard E. Sebastian, Florida 5 18 730 Athanasia Faure, 20 Jun 11 2 41 cm f/4.5 Newtonian USA Hudgens, 30 Jun 2 2

Faure, Gerard Col de l'Arzelier, 6 22 736 Harvard Pryal, 20 Sep 10-11 2 8 cm binoculars France and environs 20 cm Celestron 758 Mancunia Pryal, 20 Jan 16-17 2

40 cm Meade LX200 994 Otthild Pryal, 20 Oct 5 2

Harvey, G. Roger Concord, North 116 448 1063 Aquilegia Harvey, 73 Nov 8 3 73 cm Newtonian Carolina, USA 55 cm Dobsonian and environs 1106 Cydonia Hudgens, 30 Apr 12 2

35 cm Celestron S-C 1367 Nongoma Hudgens, 30 Jul 1 2 20 cm Dobsonian 1505 Koranna Hudgens, 30 Jul 1 2 Hudgens, Ben Stephenville, TX 11 22 30 cm f/4.9 Dobsonian USA and environs 1782 Schneller Harvey, 73 Aug 12 3

1909 Alekhin Hudgens, 30 Jul 1 2 Pryal, Jim Ellensburg, WA 34 78 20 cm f/10 Schmidt- USA and environs 2173 Maresjev Harvey, 73 Sep 28 3 Cassegrain 2325 Chernykh Harvey, 73 Sep 3 3

Rayon, Jean-michel Col de l'Arzelier, 2 5 2441 Hibbs Harvey, 73 Oct 2 6 0.6f @16.1 8 cm binoculars France and environs 40 cm Meade LX200 2506 Pirogov Harvey, 73 Feb 2 3

Watson, William W. Tonawanda, NY USA 8 35 2546 Libitina Hudgens, 30 Apr 12 2

20 cm Celestron 2568 Maksutov Hudgens, 30 Jul 1 2

2667 Oikawa Harvey, 73 Nov 3 3

2684 Douglass Harvey, 73 Feb 4 3

3058 Delmary Harvey, 73 Nov 3 3 0.5f @15.8

3201 Sijthoff Harvey, 73 Mar 9 3

3257 Hanzlík Harvey, 73 Sep 8 3

Minor Planet Bulletin 41 (2014) 190

OBSERVER & OBSERVING NO. OBSERVER & OBSERVING NO. PLANET APERTURE (cm) PERIOD (2012) OBS. PLANET APERTURE (cm) PERIOD (2012) OBS.

3330 Gantrisch Harvey, 73 Oct 2 3 11574 d'Alviella Harvey, 73 Aug 12 3

3480 Abante Harvey, 73 Apr 13 3 11734 1998 KM55 Harvey, 73 Dec 28 3

3520 Klopsteg Harvey, 73 Apr 13 3 14309 Defoy Harvey, 73 Oct 5 3

3581 Alvarez Hudgens, 30 Jul 9 2 14720 2000 CQ85 Harvey, 73 Mar 10 3

3626 Ohsaki Harvey, 73 Aug 12 3 15286 1991 RJ22 Harvey, 73 Sep 8 3

3739 Rem Hudgens, 30 Jul 9-10 2 15953 1998 BD8 Harvey, 73 Sep 8 3

3758 Karttunen Harvey, 73 Dec 28 6 16896 1998 DS9 Harvey, 73 Aug 4 3

3914 Kotogahama Harvey, 73 Sep 4 3 17188 1999 WC2 Harvey, 73 Jun 16 6

3961 Arthurcox Harvey, 73 Aug 12 3 20210 1997 GQ7 Harvey, 73 Nov 8 3

3968 Koptelov Harvey, 73 Sep 8 3 20421 1998 TG3 Harvey, 73 Oct 5 3

3992 Arthurcox Harvey, 73 Sep 7 3 21053 1990 VE Harvey, 73 Nov 28 3

4022 Nonna Harvey, 73 Aug 4 3 22110 2000 QR7 Harvey, 73 Nov 24 3

4278 Harvey Harvey, 73 Nov 24-30 10 22331 1992 AC1 Harvey, 73 Jan 5 3

4333 Sinton Harvey, 73 Aug 4 3 24367 2000 AC126 Harvey, 73 Aug 12 3

4367 Meech Harvey, 73 Oct 2 3 24445 2000 PM8 Harvey, 73 Aug 31 6

4517 Ralpharvey Harvey, 73 Oct 2 3 24827 Maryphil Harvey, 73 Aug 31 3

4626 Plisetskaya Harvey, 73 Mar 9 3 25886 2000 SY181 Harvey, 73 Jan 5 6

4709 Ennomos Harvey, 73 Nov 24 3 29156 1989 CH Harvey, 73 Feb 2 3

5001 EMP Harvey, 73 Aug 31 3 29826 1999 DW6 Harvey, 73 Jan 5 3

5431 Maxinehelin Harvey, 73 Aug 4 3 31498 1999 CX61 Harvey, 73 Aug 31 6

5683 Bifukumonin Harvey, 73 Sep 28 3 31947 2000 GO109 Harvey, 73 Sep 8 3

5744 Yorimasa Harvey, 73 Nov 28 3 0.5f @15.7 33896 2000 KL40 Harvey, 73 Jan 21 3

5813 Eizaboro Harvey, 73 May 2 3 37424 2001 YA3 Harvey, 73 Nov 8 3

5831 Dizzy Harvey, 73 Apr 14 3 38057 1999 BO15 Harvey, 73 Nov 9 3

5886 Rutger Harvey, 73 Nov 24 3 0.5f @15.7 39317 2001 UU168 Harvey, 73 Nov 3 3

5922 Shouichi Harvey, 73 Nov 8 3 46992 1998 TZ17 Harvey, 73 Jan 19 3

5934 Mats Harvey, 73 Nov 3 3 0.5f @15.7 52762 1998 MT24 Harvey, 73 Jan 5 6

6063 Jason Harvey, 73 Oct 26 6 53435 1999 VM40 Harvey, 73 Nov 29 6

6070 Rheinland Harvey, 73 Nov 28 3 68216 2001 CV26 Harvey, 73 Mar 9 6

6246 Komurotoru Harvey, 73 Nov 24 3 137126 1999 CF9 Harvey, 73 Aug 27 6

6479 Leoconnolly Harvey, 73 Mar 10 3 137805 1999 YK5 Harvey, 73 Feb 1 6

6497 Yamasaki Harvey, 73 Sep 29 - Oct 2 3 0.5f @15.7 138095 2000 DK79 Harvey, 73 Nov 14 6

6867 Kuwano Harvey, 73 May 15 6 142781 2002 UM11 Harvey, 73 Nov 3 6

7132 Casulli Harvey, 73 Mar 4 3 163364 2002 OD29 Harvey, 35 May 31 6

7167 Laupheim Harvey, 73 Oct 26 3 242643 2005 NZ6 Harvey, 73 May 1 6

7234 1986 QV3 Harvey, 73 Aug 27 3 251346 2007 SJ Harvey, 73 Nov 24 6

7291 Hyakutake Harvey, 73 Nov 4 3 277475 2005 WK4 Harvey, 73 Aug 10 6

7297 1992 UG Harvey, 73 Nov 8 3 285263 1998 QE2 Harvey, 35 May 31 6 Hudgens, 30 Jun 1 2 7355 Bottke Harvey, 73 Nov 8 3 Pryal, 20 Jun 1-5 11 Watson, 20 Jun 4 16 7419 1991 PN13 Harvey, 73 Oct 2 3 329437 2002 OA22 Harvey, 73 Sep 15 6 7858 Bolotov Harvey, 73 Sep 28 3 343098 2009 DV42 Harvey, 73 Jan 19 6 7876 1991 VW3 Harvey, 73 Oct 5 3 349068 2006 YT13 Harvey, 73 Jan 19 6 7888 1993 UC Harvey, 55, 73 Apr 6-14 12 Hudgens, 30 Apr 12 2 361071 2006 AO4 Faure, 40 Aug 11 2

8367 Bokusui Harvey, 73 Nov 24 3 2010 CL19 Harvey, 73 Nov 30 6

8504 1990 YC Harvey, 73 Nov 28 3 2010 XZ67 Harvey, 73 Dec 28 6

8651 Alineraynal Harvey, 73 Sep 29 3 2012 DA14 Faure, 20 Feb 15 10 Harvey, 20 Feb 16 6 8931 Hirokimatsuo Harvey, 73 Oct 2 3 Pryal, 20 Feb 16 3

8993 Ingstad Harvey, 73 Aug 12 3 2013 AU27 Harvey, 73 Jan 13 6

9016 Henrymoore Harvey, 73 Jan 19 6 2013 BE19 Harvey, 73 Feb 1 6

9067 Katsuno Harvey, 73 Oct 2 3 2013 ET Harvey, 73 Mar 8 6

9199 1993 FO1 Harvey, 73 Oct 5 3 2013 NJ Harvey, 73 Nov 30 6

9460 McGlynn Harvey, 73 Nov 24 3 2013 QR1 Harvey, 73 Aug 25 6

9595 1991 RE11 Harvey, 73 Jan 21 3

9693 Bleeker Harvey, 73 Oct 5 3

9936 Al-Biruni Harvey, 73 Aug 27 3

10419 1998 XB4 Harvey, 73 Feb 2 3

11131 1996 VO30 Harvey, 73 Nov 8 3

11407 1999 CV50 Harvey, 73 Sep 5 6

Minor Planet Bulletin 41 (2014) 191

TARGET ASTEROIDS! OBSERVING TARGETS FOR Asteroid Peak V Time of Peak JULY THROUGH SEPTEMBER 2014 Number Name Mag Brightness (138911) 2001 AE2 20.3 late Sep Carl Hergenrother and Dolores Hill (141018) 2001 WC47 19.9 late Sep (173664) 2001 JU2 21.6 early Jul Lunar & Planetary Laboratory (190491) 2000 FJ10 19.9 mid Aug University of Arizona (292220) 2006 SU49 19.8 early Jul 1629 E. University Blvd. (382745) 2003 CC 20.8 early Aug Tucson, AZ 85721 USA 1996 FO3 21.2 late Sep 2001 QC34 20.2 early Jul (Received: 15 April) 2002 TD60 21.4 late Sep

The V < 20 selected targets are split up into four sections: 1) Asteroids to be observed by the Target Asteroids! Carbonaceous Target Asteroids! List objects, 2) Target Asteroids! program during the period of July to September 2014 are List objects of unknown type, 3) Non-carbonaceous Target presented. In addition to asteroids on the original Target Asteroids! List objects, and 4) Other asteroids analogous to the Asteroids! list of easily accessible spacecraft targets, an OSIRIS-REx target Bennu or provide an opportunity to fill some effort has been made to identify other asteroids that are of the gaps in our knowledge of Bennu (examples include very low 1) brighter and easier to observe for small telescope and high phase angle observations, phase functions in different users and 2) analogous to (101955) Bennu, the target filters and color changes with phase angle). asteroid of the OSIRIS-REx sample return mission. The ephemerides listed below are just for planning purposes. In order to produce ephemerides for your observing location, date and Introduction time, please use the Minor Planet Center’s Minor Planet and Comet Ephemeris Service: The Target Asteroids! program strives to engage telescope users of all skill levels and telescope apertures to observe asteroids that are http://www.minorplanetcenter.net/iau/MPEph/MPEph.html viable targets for robotic sample return. The program also focuses on the study of asteroids that are analogous to (101955) Bennu, the or the Target Asteroids! specific site created by Tomas Vorobjov target asteroid of the NASA OSIRIS-REx sample return mission. and Sergio Foglia of the International Astronomical Search Most target asteroids are near-Earth asteroids (NEA) though Collaboration (IASC) at observations of relevant Main Belt asteroids may also be requested. http://iasc.scibuff.com/osiris-rex.php

Even though many of the observable objects in this program are Carbonaceous Target Asteroids! List objects faint, acquiring a large number of low S/N observations allows many important parameters to be determined. For example, an None this quarter. asteroid’s phase function can be measured by obtaining photometry taken over a wide range of phase angles. The albedo Target Asteroids! List objects of unknown type can be constrained from the phase angle observations, as there is a 1994 CJ1 (a = 1.49 AU, e = 0.32, i = 2.3°, H = 21.4) direct correlation between phase function and albedo (Belskaya 1994 CJ1 is a low delta-V asteroid that has not been well and Shevchenko, 2010) The absolute magnitude can be estimated characterized. In fact, no lightcurve, color, or phase results have by extrapolating the phase function to a phase angle of 0°. By been published for it. It will peak at V = 18.3 in early July. combining the albedo and absolute magnitude, the size of the Between early June and early August, its phase angle will range object can be estimated. from 89° to 29°. An absolute magnitude of 21.3 suggests the An overview of the Target Asteroids! program can be found at possibility of rapid (>2 h) rotation. Hergenrother and Hill (2013). DATE RA DEC ∆ r V PH Elong 07/01 14 57.9 +11 19 0.09 1.06 18.4 59 115 Quarterly Targets 07/11 16 30.7 +00 32 0.11 1.09 18.3 42 133 07/21 17 35.5 -07 22 0.14 1.13 18.7 33 142 Target Asteroids! objects brighter than V = 20.0 are presented in 07/31 18 18.9 -12 15 0.19 1.17 19.3 29 145 detail. A short summary of our knowledge of each asteroid and 10- 08/10 18 50.5 -15 11 0.24 1.22 19.9 30 144 day (shorter intervals for objects that warrant it) ephemerides are presented. The ephemerides include rough RA and Dec positions, Non-carbonaceous Target Asteroids! List objects distance from the Sun in AU (r), distance from Earth in AU (Δ), V magnitude, phase angle in degrees (PH) and elongation from the 3361 Orpheus (a = 1.21 AU, e = 0.32, i = 2.7°, H = 19.0) Sun in degrees (Elong). Much is already known about Orpheus. It is a V-type asteroid on a low delta-V orbit with a rotation period of 3.6 h and lightcurve We ask observers with access to large telescopes to attempt amplitude of ~0.3 magnitudes. With a high albedo of 0.36, this V- observations of asteroids that are between V magnitude ~20.0 and type asteroids is ~0.35 km in diameter. Target Asteroids! members ~22.0 during the quarter (contained in the table below). have been observing Orpheus since late 2013. The current quarter provides an opportunity to extend our phase angle coverage of Orpheus to low phase angles.

Minor Planet Bulletin 41 (2014) 192

DATE RA DEC ∆ r V PH Elong (243566) 1995 SA (a = 2.46 AU, e = 0.64, i = 19.9°, H = 17.4) 07/01 18 10.2 -14 54 0.47 1.48 18.8 7 169 The WISE infrared space observatory observed 1995 SA and 07/11 17 50.2 -15 33 0.52 1.51 19.3 14 158 found a low albedo of ~0.09 suggesting a possible carbonaceous 07/21 17 36.9 -16 16 0.58 1.53 19.8 21 146 07/31 17 30.4 -17 01 0.66 1.55 20.3 27 135 nature. The phase angle reached a maximum of 111° in mid-April and will decrease to a minimum of 11° in late August. Target (137799) 1999 YB (a = 1.32 AU, e = 0.07, i = 6.8°, H = 18.5) Asteroids! members have already contributed a number of This ~0.6 km near-Earth asteroid has a low relative delta-V. photometric observations. Spectroscopy has identified it as an Sq-type object. No lightcurve photometry has been published for it. It’s phase angle ranges from DATE RA DEC ∆ r V PH Elong 07/01 22 32.5 +33 51 0.53 1.23 18.4 54 100 50° at the start of the period to 6° in early October. 07/11 22 23.5 +29 48 0.54 1.32 18.3 45 112 07/21 22 11.2 +24 51 0.56 1.41 18.3 36 125 DATE RA DEC ∆ r V PH Elong 07/31 21 56.8 +19 03 0.58 1.50 18.2 26 138 07/01 00 29.0 -10 06 0.72 1.31 20.3 50 96 08/10 21 42.7 +12 45 0.63 1.59 18.2 18 151 07/11 00 48.6 -08 34 0.68 1.32 20.1 49 100 08/20 21 30.7 +06 36 0.70 1.68 18.4 12 160 07/21 01 05.6 -07 16 0.64 1.33 19.9 47 105 08/30 21 22.1 +01 09 0.79 1.77 18.7 11 160 07/31 01 19.5 -06 14 0.59 1.34 19.7 45 111 09/09 21 17.3 -03 17 0.91 1.86 19.3 14 152 08/10 01 29.5 -05 28 0.54 1.35 19.5 41 118 09/19 21 16.2 -06 41 1.05 1.94 19.8 18 143 08/20 01 34.7 -05 00 0.50 1.36 19.2 37 125 09/29 21 18.3 -09 11 1.20 2.03 20.3 21 133 08/30 01 34.1 -04 48 0.46 1.37 18.8 31 134 09/09 01 26.7 -04 48 0.43 1.38 18.5 24 146 09/19 01 12.8 -04 52 0.41 1.39 18.1 15 158 (276049) 2002 CE26 (a = 2.23 AU, e = 0.56, i = 47.2°, H = 16.8) 09/29 00 53.9 -04 46 0.40 1.40 17.8 7 169 This near-Earth asteroid is presumed to be carbonaceous due to its low albedo of 0.03 based on WISE observations. It is also a binary Other Asteroids Analogous to the OSIRIS-REx Target Bennu asteroid whose primary rotates in 3.293 h with a very small 0.06 magnitude amplitude. 112 Iphigenia (a = 2.43 AU, e = 0.13, i = 2.6°, H = 9.8) Iphigenia is a ~70-80 km carbonaceous asteroid located in the DATE RA DEC ∆ r V PH Elong inner Main Belt. Its orbit is similar to those of the Polana and 07/01 21 40.6 +44 27 1.09 1.62 19.6 38 100 07/11 21 46.0 +46 10 0.94 1.54 19.2 39 104 Eulalia carbonaceous families and Iphigenia may be related to 07/21 21 49.2 +47 22 0.79 1.47 18.7 41 108 these families and to the OSIRIS-REx target asteroid Bennu 07/31 21 49.5 +47 39 0.64 1.39 18.2 42 112 (Walsh et al., 2013). 08/10 21 46.7 +46 18 0.49 1.31 17.5 43 118 08/20 21 40.2 +41 28 0.34 1.24 16.5 41 126 Quite a bit is known about Iphigenia. It has a dark 0.039 albedo, a 08/30 21 29.0 +26 25 0.20 1.17 15.0 33 141 hydrated Ch taxonomy, and a slow rotation period of ~31.4 h. During the July-September quarter, its phase angle spans from 22° 09/04 21 20.9 +08 00 0.15 1.14 14.0 23 153 09/09 21 09.7 -23 18 0.12 1.11 13.8 30 146 to a minimum of 0.2° on August 11. 09/14 20 52.3 -55 08 0.14 1.09 14.7 53 120 09/19 20 18.6 -74 15 0.19 1.06 15.8 68 101 DATE RA DEC ∆ r V PH Elong 09/24 18 39.9 -83 58 0.26 1.04 16.5 75 91 07/01 21 47.8 -14 45 1.33 2.17 13.1 19 135 09/29 13 40.6 -86 04 0.32 1.02 17.1 77 84 07/11 21 45.9 -14 45 1.25 2.16 12.9 15 145 07/21 21 41.0 -14 56 1.19 2.15 12.6 11 155 (285944) 2001 RZ11 (a = 2.19 AU, e = 0.50, I = 53.1°, H = 16.4) 07/31 21 33.5 -15 18 1.14 2.14 12.3 6 167 08/10 21 24.5 -15 44 1.13 2.14 11.9 0 179 2001 RZ11 will be one of the brightest near-Earth asteroids this 08/20 21 15.1 -16 09 1.13 2.13 12.2 5 170 summer. The asteroid starts the period deep in the southern sky at 08/30 21 06.8 -16 28 1.16 2.13 12.5 10 158 phase angles up to 70°. On August 18, it will peak at magnitude V 09/09 21 01.0 -16 36 1.21 2.13 12.7 15 147 = 12.0 and reach a minimum phase angle of 11° as the asteroid 09/19 20 58.3 -16 33 1.28 2.12 13.0 19 137 rockets to the north. 09/29 20 58.8 -16 18 1.36 2.12 13.2 22 127 DATE RA DEC ∆ r V PH Elong 635 Vundtia (a = 3.14 AU, e = 0.08, i = 11.0°, H = 9.0) 07/01 05 00.2 -53 06 0.73 1.14 18.2 61 79 As with most large Main Belt asteroids, a lot is known about 07/11 04 54.0 -53 23 0.60 1.10 17.8 65 82 Vundtia such as its taxonomy (either a C- or B-type), low albedo 07/21 04 40.8 -54 25 0.45 1.09 17.3 69 86 (0.045) and diameter (~98 km). It has a long rotation period that is 07/31 04 06.8 -56 50 0.30 1.08 16.4 69 94 estimated to be around 11.8 h in length with a low 0.15-0.30 08/10 01 46.5 -59 40 0.15 1.09 14.5 57 115 magnitude amplitude. Vundtia can be observed from an extreme 08/14 23 18.6 -50 47 0.10 1.09 13.2 38 138 minimum phase angle of 0.04° on September 26 UT. A peak 08/18 21 06.0 -19 46 0.09 1.10 12.0 11 168 brightness of V = 13.0 is also reached on that date. 08/22 19 57.0 +09 08 1.12 1.11 13.5 34 142 08/26 19 22.3 +22 59 0.18 1.12 14.6 47 126 DATE RA DEC ∆ r V PH Elong 07/01 00 15.1 +05 30 2.78 3.01 14.6 20 93 08/30 19 03.1 +29 41 0.24 1.14 15.5 52 116 07/11 00 21.2 +05 56 2.64 3.01 14.5 19 101 09/09 18 42.6 +36 30 0.40 1.18 16.8 55 105 07/21 00 25.8 +06 08 2.50 3.00 14.3 18 110 09/19 18 38.1 +39 00 0.56 1.22 17.5 54 99 07/31 00 28.6 +06 07 2.37 2.99 14.2 17 119 09/29 18 40.8 +40 13 0.71 1.28 18.1 51 95 08/10 00 29.4 +05 50 2.26 2.99 14.0 16 128 08/20 00 28.2 +05 16 2.15 2.98 13.8 13 138 References 08/30 00 25.1 +04 26 2.07 2.98 13.6 10 149 09/09 00 20.2 +03 21 2.00 2.97 13.4 6 160 Belskaya, I., Shevchenko, V. (2000). “The Opposition Effect of 09/19 00 14.2 +02 06 1.97 2.97 13.1 2 172 09/29 00 07.5 +00 45 1.96 2.96 13.0 1 176 Asteroids.” Icarus 147, 94-105.

Minor Planet Bulletin 41 (2014) 193

Hergenrother, C., Hill, D. (2013). “The OSIRIS-REx Target Walsh, K., Delbo, M., Bottke, W., Vokrouhlicky, D., Lauretta, D. Asteroids! Project: A Small Telescope Initiative to Characterize (2013). “Introducing the Eulalia and New Polana Asteroid Potential Spacecraft Mission Target Asteroids.” Minor Planet Families: Re-assessing Primitive Asteroid Families in the Inner Bulletin 40, 164-166. Main Belt.” Icarus 225, 283-297.

ROTATION PERIOD DETERMINATION FOR We obtained a considerably high value for the amplitude: A = 0.81 7966 RICHARDBAUM ± 0.09 mag. The amplitude error was derived from the dispersion of data points near the lightcurve extrema. Alexander Kurtenkov Department of Astronomy, University of Sofia, 5 James Bourchier Blvd., Sofia 1164, BULGARIA [email protected]

Evgeni P. Ovcharov Department of Astronomy, University of Sofia, Sofia, BULGARIA

(Received: 15 April Revised: 22 May)

Photometric observations of main-belt asteroid 7966 Richardbaum were carried out in 2014 February. A synodic rotation period of 4.680 ± 0.008 h with an amplitude of 0.81 ± 0.09 mag was found.

A field near the ecliptic was imaged on 3 consecutive nights (2014 Feb 04 – 06) at the Rozhen National Astronomical Observatory (41°42′N 24°44′E) as a part of a blazar monitoring program. A Acknowledgements total of 208 frames in Cousins R filter were obtained with the 50/70-cm Schmidt telescope (f/3.44) and an FLI PL 16803 CCD This work was supported by grant No. DDVU02/40/2010 of the camera. The duration of each exposure was 300 s. Asteroid 7966 Bulgarian Science Foundation. We gratefully acknowledge Richardbaum was identified in the field using Minor Planet observing grant support from the Institute of Astronomy and Center’s MPChecker. Differential magnitudes were calculated on Rozhen National Astronomical Observatory, Bulgarian Academy the basis of 2 reference stars with a standard error of 4 mmag. The of Sciences. aperture radius was set at 5.5 arcseconds which yielded a final error in the range of 0.04 – 0.06 mag. The -5*log(rΔ) term changes References by 6 mmag over the three nights of observation which is negligible compared to the photometric error. All image processing was done Image Reduction and Analysis Facility (IRAF). using IRAF (Image Reduction and Analysis Facility). http://iraf.noao.edu

Minor Planet Center (2014). http://www.minorplanetcenter.net/

Stellingwerf, R.F. (1978). “Period determination using phase dispersion minimization.” Astrophysical Journal 224, 953-960.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid lightcurve database.” Icarus 202, 134-146, and the up-to-date version available at http://www.minorplanet.info/lightcurvedatabase.html

As of 2014 April there is no lightcurve or rotation period information for 7966 Richardbaum in the Asteriod Lightcurve Database (LCDB, Warner et al. 2009). The synodic rotation period was derived using the Phase Dispersion Minimization (PDM) technique (Stellingwerf 1978). A plot of the Θ statistic as a function of period is presented. A best fit (Θmin) was obtained at P = 4.680 ± 0.008 h.

Minor Planet Bulletin 41 (2014) 194

A NEW ASTROMETRIC MASS ESTIMATE Asteroid Mass / MS Asteroid Mass / MS FOR 121 HERMIONE 1 Ceres 4.757 E-10 16 Psyche 1.140 E-11 2 Pallas 1.010 E-10 31 Euphrosyne 2.920 E-11 Mike Kretlow 3 Juno 1.440 E-11 52 Europa 1.139 E-11 ROTAT / SATINO Observatory (C95) 4 Vesta 1.300 E-10 511 Davida 1.896 E-11 Rittergut 1 10 Hygiea 4.358 E-11 704 Interamnia 1.950 E-11 27389 Lauenbrück, Germany 15 Eunomia 1.597 E-11 121 Hermione TBD [email protected] Table 2. Perturbing asteroids and their masses (Baer and Chesley 2011) used in the dynamical model. (Received: 15 April) Dynamical model and mathematical procedure

By applying the astrometric mass determination The numerical integration was carried out using an n-body technique, a value of M = 2.4 ± 0.4 × 10–12 solar masses program developed by the author. Perturbations by the major has been obtained for the binary asteroid 121 Hermione planets Mercury – Neptune (masses and state vectors from JPL from the motion of 278 Paulina and 5750 Kandatai. DE421 ephemeris) and 11 asteroids (Table 2) were taken into account, as well as relativistic effects according to the Schwarzschild metric in isotropic coordinates (Sitarski, 1983). This paper presents a refinement of a previous work on the mass of 121 Hermione (Kretlow, 2005). The mass of the perturbing body 121 Hermione was determined by means of a Least-Squares-Fit of the solve-for parameters to the 121 Hermione. The asteroid was discovered on 1872 May 12 by observations of the test asteroid by solving the system of linear J.C. Watson at Ann Arbor. As a member of the Cybele group, equations Hermione’s orbit is located in the outer main-belt region (a = 3.45 AU, e = 0.13). The taxonomy class is C in the Tholen scheme. In , 2002 September, a satellite (diameter about 32 km), S/2002 (121) 1, was discovered with the Keck II (AO) telescope (Merline et al., where is the matrix depending on the partial 2002). derivatives of the observed coordinates with respect to the six The published diameter measurements and estimates cover the rectangular initial values of the test asteroid. is range from about 165 km effective diameter up to about 210 km, the matrix depending on the partial derivatives of the coordinates e.g. 209 km (IRAS / SIMPS: Tedesco et al., 2002), 187 km of the perturbed asteroid with respect to the perturbing mass M. R (Descamps et al., 2009), 194 km (AKARI / AcuA: Usui et al., is the matrix depending on the (O-C) residuals in coordinates of 2011), 165 km (WISE: Mainzer et al., 2011), 166 km (Marchis et the perturbed body. ΔE = (ΔE1,…,ΔE6) are the corrections to the al., 2012). The shape of the body can be described as bifurcated six initial values of the perturbed body and ΔM is the correction to and elongated. the mass of the perturbing body.

Test asteroids. In order to proof whether new test asteroid The partial derivatives P,Q were derived by integrating a set of candidates are available since the 2005 author’s work, all seven differential equations together with the equations of motion numbered asteroids where checked for mutual encounters by of the test asteroid (Sitarski, 1971). integrating each test asteroid over its observations arc span together with 121 Hermione, all major planets and the big three Data, results and discussion asteroids Ceres, Pallas and Vesta. No other suitable candidates were found. However there is a significant increase in both arc Data pre-processing for 278 Paulina and 5750 Kandatai started span and number of observations for 276 Paulina and 5750 with an apriori rejection of all semi-accurate observations (in case Kandatai since 2005. Therefore recalculations using these of 278 Paulina). additional data were done, achieving a satisfying improvement of the previous results. For all those (usually photographic) observations, which were converted by the Minor Planet Center (MPC) from FK4/B1950 to Circumstances of the encounters are given in Table 1. The mean FK5/J2000 by a global rotation (Flag ’A’ in column 15 of the diameter of a test asteroid was taken either from the IRAS / SIMPS current MPC observation format), zonal corrections FK5–FK4 catalog (Tedesco et al., 2002) for 276 Paulina or was estimated were applied (Schwan, 1988). In a second step, all FK5-based from the absolute magnitude H = 11.9 mag in the case of 5750 observations (either already processed by the former step or which Kandatai, where no further physical parameters were found in the were reduced using a FK5-based secondary catalog, e.g. PPM), or literature / databases, by the formula those which have been obtained before 1998, were transformed to the Hipparcos Catalog Reference System (HCRS) by a global rotation and subsequent correction for local differences between (p = 0.1). the Hipparcos and FK5 catalog (Mignard and Froeschlé, 2000). No further catalog debiasing (or weighting) was applied.

Encounter date Asteroid d / AU v / km s–1 D / km The total number of used observations with weight p > 0 and the 1944 Jul 28.33 278 Paulina 0.0022 2.88 35.0 number of covered oppositions in the computational run as well as 1982 Jun 08.98 5750 Kandatai 0.0009 4.54 17.5 the RMS value of the final fit and the resulting mass of the binary Table 1. Encounter circumstances for both test asteroids. d is the system 121 Hermione are given in Table 3. From these two mutual distance between the test asteroid and 121 Hermione for the individual mass estimates an averaged mean value of M = 2.4 ± 0.4 encounter date, v is the relative velocity between them during the × 10–12 solar masses has been obtained for 121 Hermione. The encounter and D is the mean diameter of the test asteroid. calculated bulk density is 1.39 ± 0.27 g/cm3 for an effective Minor Planet Bulletin 41 (2014) 195 diameter of 187 ± 6 km and 2.03 ± 0.39 g/cm3 respectively for a Observations of Main Belt Asteroids.” The Astrophysical Journal diameter value of 165 ± 5 km. If we assume an average grain Letters 759, L8 (5pp). density of ~2.9 g/cm3 for a C-type asteroid (Consolmagno et al., 2008), the bulk densities yield to a macroscopic porosity of about Mignard, F., Froeschlé (2000). “Global and local bias in the FK5 52% and 30%, respectively. from the Hipparcos data.” Astron. Astrophys. 354, 732-739.

Test asteroid Used observations RMS M (Hermione) Schwan, H. (1988). “A computer program for evaluating the count (oppositions) arcsec solar masses MS analytical representation of the systematic differences between the 278 Paulina 790 (108) 0.20 2.37 ± 0.26 × 10–12 FK4 and the FK5 or other catalogues of star positions or proper 5750 Kandatai 1014 (44) 0.10 2.33 ± 0.44 × 10–12 motions.” Astron. Astrophys. 198, 363-364. Average: 2.35 ± 0.35 × 10–12 Table 3. Individual mass results for 121 Hermione. Shampine, L.F., Gordon, M.K. (1975). “Computer Solution of Ordinary Differential Equations: the Initial Value Problem.” W. H. Conclusion Freeman and Co., San Francisco.

The mass of 121 Hermione was estimated from the analysis of the Sitarski, G. (1971). “Correction of Cometary Orbits Including the motion of the asteroids 278 Paulina and 5750 Kandatai. An Perturbations in Differential Coefficients.” Acta Astronomica 21, –12 averaged mass value M = 2.4 ± 0.4 × 10 solar masses was 87-100. –12 obtained from that. The value M = 3.3 ± 1.1 × 10 MS which was found by the author in the previous work (Kretlow, 2005) is still Sitarski, G. (1983). “Effects of General Relativity in the Motion of consistent with these new value within the formal errors. This Minor Planets and Comets.” Acta Astronomica 33, 295-304. independent solution is in a good agreement with the mass value derived from the motion of Hermione’s satellite, M = 2.36 ± 0.10 × Tedesco, E.F., Noah, P.V., Noah, M., Proce, S.D. (2002). “The –12 10 MS, by Descamps et al. (2009), which was based on an Supplemental IRAS Minor Planet Survey (SIMPS).” Astronomical effective diameter 187 ± 6 km. Journal 123, 1056-1085.

References Usui, F., Kuroda, D., Müller, T.G., Hasegawa, S., Ishiguro, M., Ootsubo, T., Ishihara, D., Kataza, H., Takita, S., Oyabu, S., Ueno, Baer, J., Chesley, S.R., Matson, R.D. (2011). “Astrometric Masses M., Matsuhara, H., Onaka, T. (2011). “Asteroid Catalog Using of 26 Asteroids and Observations on Asteroid Porosity.” Akari: AKARI/IRC Mid-Infrared Asteroid Survey.” Publications Astronomical Journal 141, 143-155. of the Astronomical Society of Japan 63, 1117-1138.

Consolmagno, G., Britt, D., Macke, R. (2008). “The significance of meteorite density and porosity.” Chemie der Erde – Geochemistry 68, 1-29. PHOTOMETRIC STUDY OF SELECTED ASTEROIDS

Descamps, P., Marchis, F., Durech, J., Emery, J., Harris, A.W., Vasilij G. Shevchenko, Feodor P. Velichko, Kaasalainen, M., Berthier, J., Teng-Chuen-Yu, J.-P., Peyrot, A., Vitaly A. Checha, Yurij N. Krugly Hutton, L., Greene, J., Pollock, J., Assafin, M., Vieira-Martins, R., Institute of Astronomy of Kharkiv Karazin National University Camargo, J.I.B., Braga-Ribas, F., Vachier, F., Reichart, D.E., Sumska Street 35, Kharkiv 61022, Ukraine Ivarsen, K.M., Crain, J.A., Nysewander, M.C., Lacluyze, A.P., [email protected] Haislip, J.B., Behrend, R., Colas, F., Lecacheux, J., Bernasconi, L., Roy, R., Baudouin, P., Brunetto, L., Sposetti, S., Manzini, F. (Received: 15 April) (2009). “New insights on the binary Asteroid 121 Hermione.” Icarus 203, 88-101. We performed photometric observations for eleven Kretlow, M. (2005). Asteroid Mass Determination. Talk given on asteroids. New rotation periods were determined for five the annual Minor Planet Meeting, Heppenheim (Germany), 2005 asteroids: 2812 Scaltriti (7.596 h), 4716 Urey (6.2 h), June 17-19. http://space.kretlow.de/? 7446 Hadrianus (3.402 h), (26657) 2000 SX293 (2.8 - Solar_System_Dynamics:Asteroid_Masses 3.8 h), and (54063) 2000 GC136 (5.154 h).

Mainzer, A., Grav, T., Masiero, J., Hand, E., Bauer, J., Tholen, D., McMillan, R.S., Spahr, T., Cutri, R.M., Wright, E., Watkins, J., Photometric observations of asteroids were carried out at the Mo, W., Maleszewski, C. (2011). “NEOWISE Studies of Chuguev Station (MPC 121) of the Institute of Astronomy Kharkiv Spectrophotometrically Classified Asteroids: Preliminary Results.” Karazin National University with a 0.7-m telescope using a one- The Astrophysical Journal 741, A90 (25pp). channel photoelectric photometer in 1995 and CCD cameras in other years. Methods of the photoelectric data reduction were Marchis, F., Enriquez, J.E., Emery, J.P., Mueller, M., Baek, M., described by Shevchenko et al. (1992); the method of CCD Pollock, J., Assafin, M., Vieira Martins, R., Berthier, J., Vachier, observations is explained in Krugly et al. (2002). The CCD-images F., Cruikshank, D.P., Lim, L.F., Reichart, D.E., Ivarsen, K.M., were reduced with the aperture photometry package (ASTPHOT) Haislip, J.B., LaCluyze, A.P. (2012). “Multiple asteroid systems: developed at DLR (Berlin) by S. Mottola (Mottola et al., 1995). Dimensions and thermal properties from Spitzer Space Telescope The observations were obtained in the V and R bands of the and ground-based observations.” Icarus 221, 1130-1161. standard Johnson-Cousins photometric system. The absolute calibrations of the comparison stars were performed with standard Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., sequences from Landolt (1992) and Skiff (2007). The accuracy of Nugent, C., Cabrera, M.S. (2012). “Preliminary Analysis of absolute photometry is equal to 0.02-0.03 mag. Our observations WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic are mainly presented as composite lightcurves which are

Minor Planet Bulletin 41 (2014) 196 constructed according to the procedures described by Harris and 7446 Hadrianus. We observed this asteroid for two apparitions in Lupishko (1989). The data are composited with the period value 2011 and 2014. We determined a rotation period of 3.402 ± shown in the figures. Data from each night, denoted by different 0.005 h. The amplitudes of the lightcurves are similar for the two symbols in the figure, were shifted along the ordinate (magnitude apparitions: A = 0.70 ± 0.02 and 0.67 ± 0.02 mag, respectively. scale) in order to obtain the best fit with the data points of other The measured color index is V-R = 0.44 ± 0.02 mag. lightcurves. The dispersion of lightcurves was used as a criterion of our combining. The accuracy of measured brightness of an (26657) 2000 SX293. This asteroid has a diameter of about 7.0 km asteroid for the individual nights is not worse than 0.03 mag. The and albedo 0.14 (Masiero et al., 2011). We observed it for one time scale is not corrected for a light time for asteroids observed night in 2007 April. The rotation period lies in range of 2.8 to 3.8 for one night. hours, if the lightcurve is symmetrical to a half period. The average amplitude of the lightcurve is A = 0.30 ± 0.05 mag. Lightcurve Observations and Rotational Periods (54063) 2000 GC136. This asteroid has a diameter of 6.5 km and 44 Nysa. There are many photometric data for this E-type asteroid albedo 0.10 (Masiero et al., 2011). It was observed for three nights (see, for example, Warner et al., 2013). Our data are consistent in 2014 March. The composite lightcurve is consistand with a with the rotation period of 6.422 ± 0.001 h found by Harris et al. rotation period of 5.154 ± 0.005 h. The maximum amplitude is A = (1989). We observed Nysa in 2011 for three nights. The composite 0.45 ± 0.03 mag. The V-R is equal to 0.47 ± 0.04 mag. lightcurve has an average amplitude A = 0.27 ± 0.03 mag. Acknowledgments 69 Hesperia. Many photometric data were obtained for this M-type asteroid (see, for example, Warner et al., 2013). We observed We are grateful to the DLR Institute of Planetary Exploration, Hesperia in 1995 March-April with a one-channel photoelectric (Germany, Berlin) for providing us the CCD-camera and the photometer. The composite lightcurve constructed with a rotation ASTPHOT software. Since 2006 June, observations on the 0.7-m period of 5.655 ± 0.005 h has an average amplitude A = 0.18 ± telescope were carried out with the CCD camera obtained thanks to 0.02 mag. INTAS grant Ref. No 03-70-567. This research was partly supported by the Ukrainian Ministry of Education and Science. 184 Dejopeja. There are many photometric data for this asteroid (see, for example, Marciniak et al., 2007; Warner et al., 2013). We References observed Dejopeja in 1995 for two nights. The composition lightcurve is constructed with a rotation period of 6.44 ± 0.01 h Harris, A.W., Lupishko, D.F. (1989). “Photometric lightcurve and has a maximum amplitude A = 0.25 ± 0.03 mag. observations and reduction techniques.” In Asteroids II (R.P. Binzel, T. Gehrels, M.S. Matthews, eds.) pp 39-53. Univ. of 212 Medea. Many photometric data were obtained for this asteroid Arizona Press, Tucson. (see, for example, Warner et al., 2013). We observed Medea in 1995 for four nights. The composite lightcurve is constructed with Harris, A.W., Young, J.W., Contreiras, L., Dockweiler, T., a rotation period of 10.288 ± 0.010 h. The average amplitude is Belkora, L., Salo, H., Harris, W.D., Bowell, E., Poutanen, M., equal to 0.15 ± 0.03 mag. Binzel, R.P., Tholen, D.J., Wang, S. (1989). “Phase relations of high albedo asteroids: the unusual opposition brightening of 44 216 Kleopatra. Many photometric data were obtained for this Nysa and 64 Angelina.” Icarus 81, 365-374. asteroid (see, for example, Warner et al., 2013). We observed Kleopatra for one night in 2013. The composite lightcurve is Krugly, Yu.N., Belskaya, I.N., Shevchenko, V.G., Chiorny, V.G., constructed with a rotation period of 5.41 ± 0.05 h. The average Velichko, F.P., Erikson, A., Mottola, S., Hahn, G., Nathues, A., Neukum, G., Gaftonyuk, N.M., Dotto, E. (2002). “CCD amplitude is equal to 0.13 ± 0.02 mag. photometry of Near-Earth asteroids in 1996-1999.” Icarus 158, 294-304. 362 Havnia. Our data are consistent with the rotation period of 16.92 ± 0.01 h found by Stephens (2009). We observed Havnia in Landolt, A. U. (1992). “UBVRI photometric standard stars in the 1996 for three nights. The composite lightcurve has an amplitude magnitude range 11.5-16.0 around the celestial equator.” Astron. J. of A = 0.17 ± 0.03 mag. 104, 340-371.

2812 Scaltriri. This asteroid has diameter about 6.1 km and high Marciniak, A., Michałowski, T., Kaasalainen, M., Durech, J., albedo 0.32 (Masiero et al., 2011) and belongs to Flora family. We Polińska, M., Kwiatkowski, T., Kryszczyńska, A., Hirsch, R., observed it for two apparitions in 2011 and 2014 and determined a Kamiński, K., Fagas, M., Colas, F., Fauvaud, S., Santacana, G., rotation period of 7.696 ± 0.010 h. There is little difference in the Behrend, R., Roy, R. (2007). “Photometry and models of selected amplitudes of the lightcurves from the two apparitions: A = 0.20 ± main belt asteroids. IV. 184 Dejopeja, 276 Adelheid, 556 Phyllis.” 0.02 and 0.25 ± 0.02 mag, respectively. We found a color index of Astron. Astrophys. 473, 633-639. V-R = 0.49 ± 0.03 mag. The high albedo of this asteroid is supposed to be E, V or Q- type, but its color index V-R is above of Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., the average for E- type (0.43 ± 0.04, Shevchenko et al., 2003). Dailey, J., Eisenhardt, P.R.M., McMillan, R.S., Spahr, T.B., This asteroid can be classified as V or Q- type object. Skrutskie, M.F., Tholen, D., Walker, R.G., Wright, E.L., DeBaun, E., Elsbury, D., Gautier, T. IV, Gomillion, S., Wilkins, A. (2011). 4716 Urey. This asteroid has diameter about 15 km and albedo “Main Belt Asteroids with WISE/NEOWISE. I. Preliminary 0.16 (Masiero et al., 2011). It was observed for one night in 2014 Albedos and Diameters.” Astropys. J. 741, 68. April. The rotation period is estimated to be about 6.2 ± 0.3 hours. Average amplitude of the lightcurve is A = 0.68 ± 0.03 mag. The Mottola, S., De Angelis, G., Di Martino, M., Erikson, A., Hahn, measured color index is V-R = 0.68 ± 0.03 mag. G., Neukum, G. (1995). “The Near-Earth objects follow-up program: first results.” Icarus 117, 62-70. Minor Planet Bulletin 41 (2014) 197

Shevchenko, V.G., Krugly, Yu.N., Chiorny, V.G., Belskaya, I.N., Gaftonyuk, N.M. (2003). “Rotation and photometric properties of E-type asteroids.” Planet. Space Sci. 51, 525-532.

Shevchenko, V.G., Chiornij, V.G., Krugly, Yu.N., Lupishko, D. F., Mohamed, R.A., Velichko, F.P., Michalowski, T., Avramchuk, V.V., Dovgopol, A.N. (1992). “Photometry of seventeen asteroids.” Icarus 100, 295-306.

Skiff, B.A. (2007). “BVRI photometry of faint field stars.” VizieR On-line Data Catalog: II/277. Originally published in: Lowell Observatory (2007).

Stephens, R.D. (2009). “Asteroids observed from GMARS and Santana observatories – April to May 2009.” Minor Planet Bul. 36, 157-158.

Warner, B.D., Harris, A.W., Pravec, P. (2013). “Asteroid Lightcurve Data Files.” http://www.minorplanet.info/lightcurvedatabase.html

Minor Planet Bulletin 41 (2014) 198

Minor Planet Bulletin 41 (2014) 199

LIGHTCURVE PHOTOMETRY OPPORTUNITIES: http://www.minorplanetcenter.net/light_curve 2014 JULY-SEPTEMBER We believe this to be the largest publicly available database of raw Brian D. Warner lightcurve data that contains 1.5 million observations for more than Center for Solar System Studies / MoreData! 2300 objects. 446 Sycamore Ave. Eaton, CO 80615 USA Lightcurve Opportunities [email protected] Objects with U = 1 should be given higher priority over those rated Alan W. Harris U = 2 or 2+ but not necessarily over those with no period. On the MoreData! other hand, do not overlook asteroids with U = 2/2+ on the La Cañada, CA 91011-3364 USA assumption that the period is sufficiently established. Regardless, do not let the existing period influence your analysis since even Petr Pravec high quality ratings have been proven wrong at times. Note that the Astronomical Institute lightcurve amplitude in the tables could be more or less than CZ-25165 Ondřejov, CZECH REPUBLIC what’s given. Use the listing only as a guide

Josef Ďurech An asterisk (*) follows the name if the asteroid is reaching a Astronomical Institute particularly favorable apparition. Charles University in Prague 18000 Prague, CZECH REPUBLIC Brightest LCDB Data # Name Date Mag Dec Period Amp U [email protected] ------926 Imhilde 07 02.1 14.3 -44 26.8 0.27 2 Lance A.M. Benner 978 Aidamina 07 03.1 14.0 +6 10.099 0.10-0.13 2 426 Hippo 07 04.9 12.6 -37 34.3 0.15-0.22 2 Jet Propulsion Laboratory 924 Toni 07 12.0 13.2 -13 21.1 0.1-0.14 1 Pasadena, CA 91109-8099 USA 838 Seraphina 07 12.1 13.8 -10 15.67 0.07-0.30 2 1343 Nicole* 07 13.3 13.7 -32 70. 0.29 1 [email protected] 1269 Rollandia 07 14.9 14.5 -20 15.4 0.02-0.13 2 982 Franklina* 07 15.1 12.6 -25 >16. 0.05 2- 1415 Malautra 07 15.2 14.4 -25 >12. 0.03 1 We present lists of asteroid photometry opportunities for 1249 Rutherfordia 07 16.2 14.4 -17 18.2 0.69-0.81 2+ 4826 Wilhelms* 07 17.5 14.3 -40 54. 1.18 2 objects reaching a favorable apparition and have no or 2569 Madeline 07 17.6 14.4 -33 0. 1 poorly-defined lightcurve parameters. Additional data on 331 Etheridgea 07 17.7 13.6 -30 13.092 0.05-0.12 2 917 Lyka 07 18.8 13.4 -29 7.92 0.14 2 these objects will help with shape and spin axis modeling 5235 Jean-Loup* 07 19.2 14.3 -15 0.09 via lightcurve inversion. We also include lists of objects 6669 Obi* 07 19.8 14.1 -34 that will be the target of radar observations. Lightcurves 3107 Weaver* 07 20.0 14.1 -19 936 Kunigunde* 07 20.8 13.5 -24 8.8 0.25 2 for these objects can help constrain pole solutions and/or 3860 Plovdiv* 07 21.3 14.3 -18 6.114 0.37 2+ remove rotation period ambiguities that might not come 1128 Astrid* 07 25.0 14.1 -21 10.228 0.29 2+ 605 Juvisia 07 25.1 13.9 -42 15.93 0.24-0.26 2 from using radar data alone. 375 Ursula 07 27.0 11.4 -33 16.83 0.04-0.17 2 1341 Edmee 07 31.8 14.0 -26 23.745 0.22-0.60 2+ 6364 Casarini* 08 01.5 14.5 -33 705 Erminia 08 04.2 13.1 -47 53.96 0.05-0.17 2 We present several lists of asteroids that are prime targets for 15673 Chetaev* 08 04.2 14.4 -19 photometry during the period 2014 July-September. 11650 1997 CN* 08 04.3 14.4 -14 739 Mandeville 08 07.3 12.4 -15 11.931 0.14 2 2554 Skiff 08 08.0 14.2 -13 In the first three sets of tables, “Dec” is the declination and “U” is 1001 Gaussia 08 09.1 14.1 -5 9.17 0.04-0.16 2- the quality code of the lightcurve. See the asteroid lightcurve data 1236 Thais 08 13.4 14.0 -42 > 72. 0.08 1 base (LCDB) documentation for an explanation of the U code: 609 Fulvia* 08 21.0 14.2 -10 > 12. 0.05 1+ 10076 1989 PK* 08 21.1 14.4 -12 2869 Nepryadva* 08 22.2 14.4 -23 0.04-0.1 http://www.minorplanet.info/lightcurvedatabase.html 795 Fini 08 23.7 14.1 -31 9.292 0.02-0.06 1+ 1114 Lorraine 08 24.1 14.2 -1 33. 0.16 1 275 Sapientia 08 25.6 13.2 -13 14.766 0.05-0.06 2 The ephemeris generator on the CALL web site allows you to 548 Kressida 08 28.9 13.7 -15 11.940 0.44 2 create custom lists for objects reaching V ≤ 18.0 during any month 1366 Piccolo* 08 30.4 13.7 -20 16.57 0.24-0.33 2 2699 Kalinin 09 04.8 14.5 -34 2.927 0.22-0.24 2+ in the current year, e.g., limiting the results by magnitude and 329 Svea 09 08.5 12.8 +0 22.77 0.09-0.26 2+ declination. 395 Delia 09 09.5 13.9 +0 19.71 0.25 2 309 Fraternitas* 09 13.1 13.4 -5 13.2 0.10-0.12 2 857 Glasenappia 09 13.5 13.3 -13 8.23 0.27-0.75 2 http://www.minorplanet.info/PHP/call_OppLCDBQuery.php 439 Ohio 09 15.3 14.4 +10 19.2 0.24 2 1424 Sundmania 09 18.2 14.0 -11 93.73 0.42 2+ We refer you to past articles, e.g., Minor Planet Bulletin 36, 188, 2525 O'Steen* 09 18.8 14.2 -6 3.55 0.19-0.22 2 314 Rosalia* 09 19.0 13.1 -3 20.43 0.21-0.40 2 for more detailed discussions about the individual lists and points 248 Lameia 09 19.9 13.3 +5 12. 0.10 2 of advice regarding observations for objects in each list. 842 Kerstin* 09 19.9 14.4 -5 1097 Vicia 09 21.5 13.6 -3 26.5 0.08 1 1271 Isergina 09 22.2 14.1 -8 Once you’ve obtained and analyzed your data, it’s important to 393 Lampetia* 09 22.5 10.7 +15 38.7 0.12-0.14 2- publish your results. Papers appearing in the Minor Planet Bulletin 791 Ani 09 24.3 12.9 -18 16.72 0.17-0.38 2 1110 Jaroslawa* 09 24.4 12.6 +12 94.432 0.44-0.80 2+ are indexed in the Astrophysical Data System (ADS) and so can be 379 Huenna* 09 24.5 11.9 +0 14.14 0.07-0.09 2 referenced by others in subsequent papers. It’s also important to 2484 Parenago* 09 24.5 13.7 +1 make the data available at least on a personal website or upon 269 Justitia 09 25.6 12.7 -3 16.545 0.14-0.25 2 784 Pickeringia 09 26.1 13.6 -2 13.17 0.20-0.40 2 request. We urge you to consider submitting your raw data to the 952 Caia* 09 30.4 11.8 -1 7.51 0.03-0.13 2 ALCDEF page on the Minor Planet Center web site:

Minor Planet Bulletin 41 (2014) 200

Low Phase Angle Opportunities with sparse data, could easily lead to the asteroid being added to DAMIT, thus increasing the total number of asteroids with spin The Low Phase Angle list includes asteroids that reach very low axis and shape models. phase angles. The “α” column is the minimum solar phase angle for the asteroid. Getting accurate, calibrated measurements Note that you can compare and combine the results of searches (usually V band) at or very near the day of opposition can provide using the ephemeris generator and LCDB query (limited to with or important information for those studying the “opposition effect.” without a pole solution) at the sites listed above to create your own customized list of objects. You will have the best chance of success working objects with low Brightest LCDB Data amplitude and periods that allow covering at least half a cycle # Name Date Mag Dec Period Amp U every night. Objects with large amplitudes and/or long periods are ------much more difficult for phase angle studies since, for proper 901 Brunsia* 07 02.2 12.5 -21 3.1363 0.11-0.28 3 552 Sigelinde* 07 02.6 13.2 -20 17.156 0.16 3 analysis, the data have to be reduced to the average magnitude of 1157 Arabia* 07 06.4 13.8 -35 15.225 0.37 3- the asteroid for each night. This reduction requires that you 881 Athene* 07 07.6 13.8 -19 13.895 0.39-0.53 3- 2474 Ruby* 07 09.6 14.0 -11 7.42 0.11-0.16 3 determine the period and the amplitude of the lightcurve; for long 1842 Hynek* 07 12.7 13.8 -14 3.941 0.10-0.17 3 period objects that can be tricky. Refer to Harris, et al. (“Phase 939 Isberga* 07 13.8 13.6 -25 2.9173 0.22-0.25 3 Relations of High Albedo Asteroids.” Icarus 81, p365 ff) for the 634 Ute* 07 20.1 13.1 -15 11.7554 0.14-0.17 3 1666 van Gent* 07 23.8 13.8 -17 4.166 0.30 3 details of the analysis procedure. 861 Aida* 07 24.6 13.2 -21 10.95 0.32 3 172 Baucis* 07 28.4 11.1 -28 27.417 0.23-0.35 3 As an aside, some use the maximum light to find the phase slope 805 Hormuthia* 08 02.7 13.4 -3 9.51 0.05 3- 794 Irenaea* 08 09.3 13.6 -12 9.14 0.40 3- parameter (G). However, this can produce a significantly different 2650 Elinor* 08 09.9 13.5 -23 2.762 0.12-0.18 3 value for both H and G versus when using average light, which is 112 Iphigenia* 08 11.1 11.8 -16 31.466 0.30 3 4150 Starr* 08 20.3 13.9 -15 4.5179 0.08-0.20 3 the method used for values listed by the Minor Planet Center. 672 Astarte* 08 23.6 14.0 -16 22.572 0.10-0.16 3 883 Matterania* 08 28.7 13.7 -2 5.64 0.36-0.42 3 # Name Date α V Dec Period Amp U 285 Regina* 09 01.8 14.0 +6 9.542 0.13-0.16 3 ------4909 Couteau* 09 02.3 14.0 -12 552 Sigelinde 07 02.7 0.98 13.3 -20 17.156 0.16 3 2292 Seili* 09 03.9 13.8 -2 5.121 0.25-0.42 3 514 Armida 07 05.8 0.50 13.1 -21 21.851 0.16-0.42 3 723 Hammonia* 09 06.1 13.7 -7 5.436 0.18 3 240 Vanadis 07 07.5 0.23 12.8 -22 10.64 0.30-0.34 3 33 Polyhymnia* 09 09.4 9.8 -7 18.608 0.13-0.21 3 334 Chicago 07 16.8 0.47 12.8 -20 7.361 0.15-0.67 3 10217 Richardcook* 09 11.8 13.9 -9 23.33 0.45 3- 49 Pales 07 20.1 0.31 11.8 -20 10.42 0.18-0.20 3 1641 Tana* 09 14.1 14.0 +1 7.95 0.32-0.33 3- 30 Urania 07 20.9 0.27 10.1 -21 13.686 0.11-0.45 3 4910 Kawasato* 09 18.5 13.6 -1 212 Medea 07 21.8 0.50 12.7 -22 10.283 0.04-0.16 3 373 Melusina* 09 23.6 12.5 -1 12.97 0.20-0.25 3 27 Euterpe 07 22.2 0.41 10.4 -21 10.4082 0.13-0.21 3 635 Vundtia* 09 26.0 12.8 +1 11.79 0.15-0.27 3 586 Thekla 07 23.5 0.71 13.6 -18 13.670 0.22-0.30 3 84 Klio* 09 26.5 10.8 +14 23.562 0.04-0.21 3 861 Aida 07 24.6 0.52 13.2 -21 10.95 0.32 3 888 Parysatis 07 27.5 0.16 13.2 -19 5.9314 0.22-0.26 3 817 Annika 07 31.0 0.25 13.7 -19 10.56 0.16-0.27 3 Radar-Optical Opportunities 147 Protogeneia 08 03.4 0.85 12.8 -15 7.8528 0.25-0.28 3 16 Psyche 08 07.1 0.51 9.3 -15 4.196 0.03-0.42 3 739 Mandeville 08 07.4 0.41 12.4 -15 11.931 0.14 2 There are several lists to help plan observations in support of radar. 112 Iphigenia 08 11.1 0.24 11.8 -16 31.466 0.30 3 243 Ida 08 17.0 0.01 13.6 -14 4.634 0.40-0.86 3 Future radar targets: 96 Aegle 08 18.2 0.42 12.3 -12 13.82 0.05-0.29 3 606 Brangane 08 18.4 0.88 12.3 -11 12.2950 0.20 3- http://echo.jpl.nasa.gov/~lance/future.radar.nea.periods.html 63 Ausonia 08 24.8 0.56 9.7 -12 9.298 0.15-0.95 3 275 Sapientia 08 25.6 0.69 13.2 -13 14.766 0.05-0.06 2 Past radar targets: 489 Comacina 09 03.3 0.66 12.8 -06 9.02 0.12-0.39 3 723 Hammonia 09 06.1 0.05 13.7 -07 5.436 0.18 3 http://echo.jpl.nasa.gov/~lance/radar.nea.periods.html 760 Massinga 09 06.8 0.96 13.3 -03 10.72 0.12-0.14 3 33 Polyhymnia 09 09.4 0.80 9.8 -07 18.608 0.13-0.20 3 Arecibo targets: 309 Fraternitas 09 13.2 0.31 13.4 -05 13.2 0.10-0.12 2 http://www.naic.edu/~pradar/sched.shtml 260 Huberta 09 16.0 0.41 13.0 -04 8.29 0.21-0.27 3 http://www.naic.edu/~pradar 4910 Kawasato 09 18.6 0.65 13.7 -01 314 Rosalia 09 19.0 0.79 13.1 -03 20.43 0.21-0.40 2 373 Melusina 09 23.7 0.60 12.5 -01 12.97 0.20-0.25 3 Goldstone targets: 379 Huenna 09 24.5 0.23 11.9 +00 14.14 0.07-0.09 2 http://echo.jpl.nasa.gov/asteroids/goldstone_asteroid_schedule.html 2484 Parenago 09 24.6 0.66 13.7 +01 635 Vundtia 09 26.0 0.04 12.8 +01 11.790 0.15-0.27 3 However, these are based on known targets at the time the list was prepared. It is very common for newly discovered objects to move Shape/Spin Modeling Opportunities up the list and become radar targets on short notice. We recommend that you keep up with the latest discoveries using the Those doing work for modeling should contact Josef Ďurech at the RSS feeds from the Minor Planet Center email address above or visit the Database of Asteroid Models from Inversion Techniques (DAMIT) web site for existing data and http://www.minorplanetcenter.net/iau/rss/mpc_feeds.html models In particular, monitor the NEA feed and be flexible with your http://astro.troja.mff.cuni.cz/projects/asteroids3D observing program. In some cases, you may have only 1-3 days when the asteroid is within reach of your equipment. Be sure to if looking to add lightcurves for objects already in the DAMIT keep in touch with the radar team if you get data (through Dr. database. Benner’s email listed above). They may not always be observing Below is a partial list of objects reaching brightest this quarter the target but, in some cases, your initial results may change their with well-determined periods and are not in the DAMIT database. plans. In all cases, your efforts are greatly appreciated. However, since they have a high U rating, this means there is at least one dense lightcurve of high quality. A second one, along Minor Planet Bulletin 41 (2014) 201

Use the ephemerides below as a guide to your best chances for (163132) 2002 CU11 (Aug-Sep, H = 18.3, PHA) observing, but remember that photometry may be possible before Thomas et al. (2014, Icarus 228, 217-246) report 2002 CU11 as a and/or after the ephemerides given below. Note that geocentric type C/X asteroid. Assuming an albedo for type C, pV = 0.057, this positions are given. Use these web sites to generate updated and gives an estimated diameter of 1.2 km. There were no lightcurve topocentric positions: parameters found.

MPC: http://www.minorplanetcenter.net/iau/MPEph/MPEph.html DATE RA Dec ED SD V α SE ME MP GB ------JPL: http://ssd.jpl.nasa.gov/?horizons 08/15 07 26.0 +79 45 0.23 0.95 18.6 99.9 67 82 -0.76 +28 08/20 06 27.7 +76 44 0.16 0.97 17.9 101.8 70 58 -0.26 +25 In the ephemerides below, ED and SD are, respectively, the Earth 08/25 05 23.0 +66 24 0.08 0.99 16.6 102.1 73 72 +0.00 +16 08/30 04 18.8 +04 51 0.03 1.01 14.0 85.4 93 139 +0.17 -31 and Sun distances (AU), V is the estimated Johnson V magnitude, 09/04 03 20.9 -62 18 0.08 1.03 15.3 68.8 107 93 +0.67 -47 and α is the phase angle. SE and ME are the great circles distances 09/09 02 31.5 -73 41 0.15 1.06 16.7 66.4 106 77 +1.00 -42 09/14 01 50.9 -77 12 0.22 1.08 17.5 64.5 104 95 -0.71 -39 (in degrees) of the Sun and Moon from the asteroid. MP is the 09/19 01 18.3 -78 33 0.30 1.11 18.1 62.6 102 107 -0.23 -38 lunar phase and GB is the galactic latitude. “PHA” in the header indicates that the object is a “potentially hazardous asteroid”, (276049) 2002 CE26 (Aug-Oct, H = 18.4, Binary) meaning that at some (long distant) time, its orbit might take it Shepard et al. (2004, IAUC 8397) using radar observations first very close to Earth. reported this NEA as being a binary. Using photometry observations, Pravec et al. (2006, Icarus 181, 63-93) reported a 2010 LE15 (Jul-Aug, H = 19.5, PHA) rotation period for the primary of 3.2930 h. The orbital period of There are known lightcurve parameters for this NEA. Its estimated the satellite was found to be 15.6 hours. The phase angle bisector diameter is about 400 meters. While possible, it’s not too likely longitude will be similar during this apparition as it was during the that it is a superfast rotator with a period of < 2 hours. time of the Pravec et al. observations. This makes it likely that mutual events (occultations or eclipses involving the satellite) will DATE RA Dec ED SD V α SE ME MP GB ------be seen. Given that possibility, high-precision observations, on the 07/15 23 09.3 +22 01 0.16 1.09 17.8 60.1 112 35 -0.90 -35 order of 0.01-0.02 mag, and – preferably – well-calibrated to at 07/20 23 23.0 +20 43 0.13 1.08 17.4 59.0 115 44 -0.40 -38 07/25 23 40.8 +18 22 0.11 1.07 16.9 57.9 117 99 -0.04 -41 least an internal system will be required. 07/30 00 06.4 +14 01 0.08 1.06 16.2 57.4 119 152 +0.08 -47 08/04 00 47.8 +05 26 0.06 1.04 15.6 58.8 118 152 +0.50 -57 DATE RA Dec ED SD V α SE ME MP GB 08/09 02 03.4 -11 37 0.04 1.03 15.1 67.7 110 95 +0.95 -67 ------08/14 04 16.3 -33 48 0.04 1.01 15.7 88.2 89 67 -0.85 -46 08/05 21 48.6 +47 16 0.56 1.35 17.9 43.1 115 105 +0.60 -5 08/19 06 36.7 -42 37 0.05 1.00 17.1 105.7 71 66 -0.35 -21 08/15 21 44.0 +44 33 0.41 1.28 17.1 42.7 121 59 -0.76 -7 08/25 21 35.3 +36 08 0.27 1.21 15.9 38.5 132 135 +0.00 -12 09/04 21 20.9 +08 00 0.15 1.14 14.0 23.8 153 55 +0.67 -28 2001 RZ11 (Jul-Sep, H = 16.4, PHA) 09/14 20 52.2 -55 10 0.14 1.08 14.7 53.6 120 110 -0.71 -39 The estimated size for this NEA is 1.6 km. It will be moving 09/24 18 39.6 -83 59 0.25 1.04 16.5 75.1 91 90 +0.00 -27 rapidly north around the middle of August. Fortunately it will be 10/04 11 19.3 -83 22 0.39 1.01 17.5 78.2 80 82 +0.74 -21 10/14 10 20.7 -78 43 0.51 0.99 18.0 76.2 74 103 -0.67 -18 very bright and so short exposures to avoid excessive trailing will be possible even for small telescopes. There are no known lightcurve parameters.

DATE RA Dec ED SD V α SE ME MP GB ------07/10 04 54.9 -53 20 0.61 1.11 17.9 65.3 82 108 +0.91 -39 07/20 04 42.7 -54 16 0.47 1.09 17.4 68.8 86 73 -0.40 -40 07/30 04 12.2 -56 30 0.32 1.08 16.5 70.0 93 98 +0.08 -44 08/09 02 13.8 -59 54 0.16 1.08 14.8 60.5 111 81 +0.95 -54 08/19 20 43.8 -10 59 0.09 1.10 12.3 15.4 163 123 -0.35 -30 08/29 19 07.0 +28 24 0.22 1.13 15.3 51.9 118 97 +0.11 +9 09/08 18 43.7 +36 07 0.38 1.17 16.7 55.8 106 64 +0.98 +17 09/18 18 38.1 +38 50 0.54 1.22 17.5 54.4 100 123 -0.32 +19

IN THIS ISSUE Number Name EP Page Number Name EP Page 236 Honoria 17 155 1019 Strackea 6 144 317 Roxane 33 171 1025 Riema 6 144 This list gives those asteroids in this issue for 323 Brucia 6 144 1044 Teutonia 1 139 which physical observations (excluding 428 Monachia 6 144 1181 Lilith 46 184 astrometric only) were made. This includes 434 Hungaria 6 144 1219 Britta 1 139 lightcurves, color index, and H-G 473 Nolli 37 175 1219 Britta 33 171 determinations, etc. In some cases, no specific 487 Venetia 46 184 1246 Chaka 46 184 results are reported due to a lack of or poor 495 Eulalia 6 144 1246 Chaka 48 186 quality data. The page number is for the first 502 Sigune 33 171 1294 Antwerpia 1 139 520 Franziska 17 155 1294 Antwerpia 33 171 page of the paper mentioning the asteroid. EP is 525 Adelaide 17 155 1299 Mertona 1 139 the “go to page” value in the electronic version. 616 Elly 1 139 1321 Majuba 1 139 616 Elly 33 171 1359 Prieska 31 169 Number Name EP Page 620 Drakonia 1 139 1360 Tarka 6 144 18 Melpomene 17 155 670 Ottegebe 33 171 1374 Isora 33 171 110 Lydia 6 144 684 Hildburg 46 184 1384 Kniertje 31 169 121 Hermione 56 194 702 Alauda 48 186 1600 Vyssotsky 6 144 155 Scylla 33 171 772 Tanete 46 184 1626 Sadeya 6 144 163 Erigone 49 187 822 Lalage 1 139 1656 Suomi 6 144 199 Byblis 1 139 822 Lalage 33 171 1943 Anteros 19 157 208 Lacrimosa 33 171 852 Wladilena 6 144 2161 Grissom 31 169 227 Philosophia 50 188 855 Newcombia 1 139 2381 Landi 1 139 234 Barbara 17 155 855 Newcombia 33 171 2381 Landi 33 171 Minor Planet Bulletin 41 (2014) 202

Number Name EP Page Number Name EP Page Number Name EP Page 2713 Luxembourg 19 157 11958 Galiani 40 178 86039 1999 NC43 19 157 2770 Tsvet 32 170 12920 1998 VM15 40 178 86217 1999 TB35 6 144 2812 Scaltriti 57 195 13026 1989 CX 40 178 87073 2000 KF66 40 178 2834 Christy Carol 46 184 13578 1993 MK 6 144 98889 2001 BL38 39 177 3062 Wren 31 169 14255 2000 AS70 40 178 113781 2002 TF188 40 178 3101 Goldberger 6 144 15374 Teta 6 144 118337 1999 BQ9 6 144 3266 Bernardus 6 144 15964 Billgray 6 144 120279 2004 HE18 40 178 3309 Brorfelde 6 144 16009 1999 CM8 39 177 138127 2000 EE14 19 157 3496 Arieso 33 171 16135 Ivarsson 40 178 143409 2003 BQ46 19 157 3573 Holmberg 1 139 16562 1992 AV1 6 144 243566 1995 SA 19 157 3800 Karayusuf 6 144 17590 1995 CG 6 144 275677 2000 RS11 19 157 3992 Wagner 39 177 19682 1999 RW194 40 178 277570 2005 YP180 19 157 4055 Magellan 19 157 20561 1999 RE120 40 178 294739 2008 CM 19 157 4067 Mikhelson 48 186 20744 2000 AO151 40 178 306695 2000 VL1 40 178 4440 Tchantches 6 144 21107 1992 PZ4 40 178 326317 1999 VN23 40 178 4464 Vulcano 6 144 21688 1999 RK37 6 144 357622 2005 EY95 19 157 4490 Bambery 6 144 22412 1995 UQ4 31 169 377097 2002 WQ4 19 157 4511 Rembrandt 39 177 24393 2000 AG183 31 169 1995 CR 19 157 4716 Urey 57 195 25916 2001 CP44 19 157 2006 DP14 19 157 4954 Eric 19 157 26022 4180 P-L 40 178 2009 CT 19 157 5175 Ables 6 144 26657 2000 SX293 57 195 2009 QF31 19 157 5253 1985 XB 6 144 28461 2000 AL164 40 178 2011 BT15 19 157 5380 Sprigg 40 178 34726 2001 QA25 40 178 2012 AU10 19 157 5450 Sokrates 40 178 35107 1991 VH 19 157 2013 PD21 19 157 5707 Shevchenko 40 178 36439 2000 PT26 40 178 2013 WT44 19 157 5871 Bobbell 6 144 40267 1999 GJ4 19 157 2013 XF22 19 157 6043 Aurochs 31 169 44600 1999 RU10 6 144 2013 XV8 19 157 6107 Osterbrock 6 144 48601 1995 BL 6 144 2013 YZ13 19 157 6493 Cathybennett 6 144 49667 1999 OM2 6 144 2013 YZ37 19 157 6516 Gruss 40 178 52317 1992 BC1 33 171 2014 AY28 19 157 6517 Buzzi 6 144 53435 1999 VM40 19 157 2014 BR57 19 157 6652 1991 SJ1 39 177 53530 2000 AV200 6 144 2014 BR8 19 157 7446 Hadrianus 57 195 54063 2000 GC136 57 195 2014 CG13 19 157 7454 Kevinrighter 40 178 55532 2001 WG2 33 171 2014 CR 19 157 7966 Richardbaum 55 193 68031 2000 YK29 19 157 2014 CU13 19 157 8866 Tanegashima 40 178 69142 2003 FL115 6 144 2014 DX110 19 157 8958 Stargazer 40 178 69406 1995 SX48 6 144 2014 EL45 19 157 9165 Raup 6 144 85118 1971 UU 40 178 2014 EM 19 157 10465 1980 WE5 40 178 85990 1999 JV6 19 157 2014 EY24 19 157

THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly Authors should submit their manuscripts by electronic mail ([email protected]). journal of the Minor Planets Section of the Association of Lunar and Author instructions and a Microsoft Word template document are available Planetary Observers (ALPO). Current and most recent issues of the MPB at the web page given above. All materials must arrive by the deadline for are available on line, free of charge from: each issue. Visual photometry observations, positional observations, any http://www.minorplanet.info/mpbdownloads.html type of observation not covered above, and general information requests Nonmembers are invited to join ALPO by communicating with: Matthew 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 Lawrence Garrett, The deadline for the next issue (41-4) is July 15, 2014. The deadline for 206 River Rd., Fairfax, VT 05454 USA ([email protected]). Dr. issue 42-1 is October 15, 2014. 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, 17995 Bakers Farm Rd., Colorado Springs, CO 80908 USA ([email protected]).

The Minor Planet Bulletin is edited by Professor Richard P. Binzel, MIT 54-410, Cambridge, MA 02139 USA ([email protected]). Brian D. Warner (address above) 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 41 (2014)