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1 LIGHTCURVES for ASTEROIDS 18301 KONYUKHOV and 2022 WEST Sinhué A.R. Haro-Corzo, Luis A. Villegas Escuela Nacional De Estudio

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1 LIGHTCURVES for ASTEROIDS 18301 KONYUKHOV and 2022 WEST Sinhué A.R. Haro-Corzo, Luis A. Villegas Escuela Nacional De Estudio 1 2 LIGHTCURVES FOR ASTEROIDS 18301 KONYUKHOV with a final field of view of 7.6 × 7.6 arcmin .​ All observations ​ AND 2022 WEST were unfiltered. The observed images were corrected using ​ standard IRAF routines in order to correct them for nightly bias, Sinhué A.R. Haro-Corzo, Luis A. Villegas dark current and flat-field effects. We used MPO Canopus Escuela Nacional de Estudios Superiores Unidad Morelia (V9.5.0.14, BDW Publishing, 2017) to carry out differential Universidad Nacional Autónoma de México photometric measurements and lightcurve analysis. Morelia, Michoacán, MÉXICO [email protected] 18301 Konyukhov (1979 QZ9) was discovered on 1979 August ​ 27 by N. S. Chernykh and was named after the Russian traveler Lorenzo Olguín, Julio C. Saucedo, María E. Contreras Fyodor Fyodorovich Konyukhov. It is an outer main-belt asteroid Departamento de Investigación en Física with H magnitude of 13.4 (see JPL Horizons webpage). The Universidad de Sonora asteroid was observed at the OAN-SPM on six nights of 2016 Hermosillo, Sonora, MÉXICO (Aug 20, 21, 22 & 23; Oct 15 & 18). During analysis, Aug 22 observations were treated as two separate sessions because the Pedro V. Sada asteroid passed in front of a bright star. A total of 395 data points Departamento de Física y Matemáticas were used to construct its lightcurve. From this curve, we derived Universidad de Monterrey an intrinsic rotation period of 2.6667±0.0003 h with an amplitude Av. I. Morones Prieto 4500 Pte. of ~0.17 mag (see Figure for 18301 Konyukhov). This period is in San Pedro Garza García, N.L. 66238 the range of a typical asteroid in the main-belt. According to the MÉXICO JPL Small-Body Database there are a total of 1738 observations Sandra A. Ayala, Jaime R. Garza (all types) since 1979. However, as far as we know there is not Facultad de Ciencias Físico-Matemáticas photometry nor lightcurve data reported in the literature. Universidad Autónoma de Nuevo León Monterrey, Nuevo León MÉXICO Juan Segura-Sosa Facultad de Ciencias Físico-Matemáticas Universidad Autónoma de Coahuila Saltillo, Coahuila, MÉXICO Claudia P. Benítez-Benítez Escuela Superior de Física y Matemáticas Instituto Politécnico Nacional Cd. de México, MÉXICO (Received: 2018 Feb 12, Accepted: 2018 May 16 ) We report photometric analysis of two main-belt asteroids observed at the Observatorio Astronomico Nacional in the Sierra San Pedro Martir, Baja California, México. For 18301 Konyukhov our derived intrinsic rotation period is 2.6667±0.0003 h with an amplitude of 0.16 magnitudes. To the best of our knowledge, this is 2022 West (1938 CK) was discovered on 1938 February 7 by K. the first lightcurve reported for this asteroid. In the case Reinmuth. It is a main-belt asteroid with H magnitude 11.6 (see of 2022 West our derived intrinsic rotation period is JPL Horizons webpage). 2022 West was reported by Franco and 14.1385 ±0.0031 h with an amplitude of 0.54 Marchini (2017) to have a rotation period of 14.14±0.01 h. In this magnitudes. work 2022 West was observed on seven nights of 2016 (Aug 20 & 21; Oct 11,15 & 18; Nov 10 & 11). During analysis, Oct 18 observations were treated as two separate sessions because two The Mexican effort to achieve coordinated simultaneous different sets of bright and comparison stars were used. A total of photometric observations of asteroids is embodied by the Mexican 287 data points were used to construct its lightcurve. Based on this Asteroid Photometric Campaign (hereafter CMFA). Since 2015, curve, we derived an intrinsic rotation period of 14.1385±0.0031 h more than 10 asteroids have been photometrically observed and with an amplitude of 0.54 mag (see Figure for 2022 West). In this analyzed (Sada et al 2016, 2017, 2018). In this work we present case, the period is 3.2 times more precise than previous works photometric data of two main-belt asteroids supplemental to the because this asteroid was observed over a longer period of time. 2016 CMFA. These objects were observed in the period 2016 August-November as targets of opportunity at the Observatorio Astronómico Nacional at San Pedro Mártir (hereafter OAN-SPM; MPC 679) in Baja California, México. The observations were carried out with the 0.84-m f/15 Ritchey-Chretien telescope. We used a 2048×2048 pix2 E2V-4240 cryogenic CCD operating at a ​ temperature of -110 °C. The images were generally binned 2 × 2 Minor Planet Bulletin 45 (2018) Number Name 2016 mm/dd Pts Phase L B Period(h) P.E. Amp A.E. Grp ​PAB ​PAB 18301 Konyukhov 08/20-10/18 395 10.9,12.7 312.4 0.69 2.6667 0.0003 0.15 0.02 MB 2022 West 08/20-11/11 287 22.5, 10.2 27.9 2.74 14.1385 0.0031 0.54 0.04 MB Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. L and B are ​PAB ​PAB the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984) which values were extracted from ​ ​ https://ssd.jpl.nasa.gov/horizons.cgi#top . Grp is the asteroid family/group (Warner et al., 2009). ​ ​ ​ “Results of the 2016 Mexican Asteroid Photometry Campaign.” Minor Planet Bulletin 44, 239-242. ​ ​ ​ Sada, P.V., Loera-González, P., L.L., Saucedo-Morales, J.C., Ayala-Gómez, S.A., Garza, J.R. (2018). “Results of the 2017 Mexican Asteroid Photometry Campaign – Part 1.” Submitted to the Minor Planet Bulletin. Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sep. http://www.minorplanet.info/lightcurvedatabase.html Warner. B.D. (2017). MPO Canopus software. http://bdwpublishing.com Acknowledgements The results presented in this report are based upon observations carried out at the Observatorio Astronómico Nacional on the Sierra San Pedro Mártir (OAN-SPM), Baja California, México. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. References Franco, L. and Marchini, A. (2017). “Rotation Periods for 1751 ​ Herget, 2022 West and (23997) 1999 RW27” Minor Planet ​ ​ ​ ​ Bulletin 44, 93-94 ​ ​ ​ JPL Horizons, Solar System Dynamics Group, Horizons On-Line Ephemeris System (2017) from https://ssd.jpl.nasa.gov/horizons.cgi#top JPL Small-Body Database Browser (2017) from https://ssd.jpl.nasa.gov/sbdb.cgi#top Sada, P.V., Navarro-Meza, S., Reyes-Ruiz, M., Olguín, L.L., Saucedo, J.C., Loera-González, P. (2016). “Results of the 2015 Mexican Asteroid Photometry Campaign.” Minor Planet Bulletin ​ 43, 154-156. ​ Sada, P.V., Olguín, L., Saucedo, J.C., Loera-González, P., Cantú-Sánchez, L., Garza, J.R., Ayala-Gómez, S.A., Avilés, A., Pérez-Tijerina, E., Navarro-Meza, S., Silva, J.S., Reyes-Ruiz, M., Segura-Sosa, J., López-Valdivia, R., Álvarez-Santana, F. (2017). Minor Planet Bulletin 45 (2018) .
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