Lorenzo Franco Balzaretto Observatory (A81), Rome, ITALY firstname.lastname@example.org
Maurizio Scardella, Angelo Tomassini,
Francesco Franceschini, Fernando Pierri
Osservatorio Astronomico “F. Fuligni” (D06)
Via Lazio 14, 00040 Rocca di Papa (RM), ITALY
Astronomical Observatory, DSFTA – University of Siena (K54)
Via Roma 56, 53100 – Siena, ITALY
(Received: 2017 Apr 5)
Collaborative lightcurve photometry observations of
main-belt asteroid 703 Noemi were made over 16 nights
in 2016 November thru 2017 January. The resulting
synodic rotation period is 200 ± 1 h, amplitude 0.62 ±
0.10 mag, HR = 12.24 ± 0.12 and GR = 0.16 ± 0.10.
The main-belt asteroid 703 Noemi was discovered on 1910 October 3 by J. Palisa at Vienna. The primary orbital elements are a = 2.175 AU, e = 0.138, and i = 2.46°. Its absolute magnitude is H = 12.5 (JPL, 2017). The NEOWISE survey (Nugent et al., 2016) used a value of 12.70 to find a diameter of D = 9.85 ± 1.42 km. The gives an optical albedo of pV = 0.19 ± 0.10. CCD photometric observations were made over 16 nights from 2016 November 15 to 2017 January 29 at the Balzaretto Observatory (A81), Fuligni Observatory, and the DSFTA Observatory (DSFTA, 2017) using the instrumentation described in Table I.
Data processing and analysis were done at the Balzaretto Observatory with MPO Canopus (Warner, 2016). All the images, acquired with clear-filter, were calibrated with dark and flat frames and converted to the Cousins-R magnitudes using solar colored field stars from CMC15 catalogue (VizieR, 2014) by the relationship R = r´ – 0.22 (Dymock and Miles, 2009). No offset adjustment was applied to the lightcurves. The period analysis shows a bimodal solution for P = 200 ± 1 hours and amplitude A = 0.62 ± 0.10 magnitudes.
The absolute magnitude H (R-band) and slope parameter G were found using the H-G Calculator function of MPO Canopus. For each lightcurve the average R mag was measured removing the rotational effects, using a Fourier fit model (Buchheim, 2010). We found H (R-band) = 12.24 ± 0.12 mag, G = 0.16 ± 0.10. For 703 Noemi, the taxonomic class and the color index are unknown. We assume it is S-type asteroid, according to SMASSII taxonomic class distribution vs semi-major axis (Bus and Binzel, 2002) with a color index V-R = 0.49 ± 0.05 (Shevchenko and Lupishko, 1998). We then derive H = 12.73 ± 0.13, close to the H = 12.7 listed by Nugent et al. (2016).
Observatory Telescope, CCD Exp (s)
Balzaretto (A81)- 0.20-m f/5.5 SCT SBIG ST7xme 420
Fuligni (D06)- 0.35-m f/10 SCT SBIG ST8-xe 120
DSFTA (K54)- 0.30-m f/5.6 MCT SBIG STL-6303e (2×2) 300
Table II. Observing Instrumentation. SCT: Schmidt-Cassegrain Telescope, MCT: Maksutov-Cassegrain Telescope.
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DSFTA (2017). Dipartimento di Scienze Fisiche, della Terra e dell’Ambiente, University of Siena – Astronomical Observatory. https://www.dsfta.unisi.it/en/department/sciencemuseums/astronomical-observatory
Dymock, R., Miles, R. (2009). “A method for determining the V magnitude of asteroids from CCD images.” J. Br. Astron. Assoc. 119, 149-156.
Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.
JPL (2017). Small-Body Database Browser. http://ssd.jpl.nasa.gov/sbdb.cgi#top Nugent, C.R., Mainzer, A., Bauer, J., Cutri, R.M., Kramer, E.A., Grav, T., Masiero, J., Sonnett, S., Wright, E.L. (2016).
“NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos.” Astron. J. 152, A63.
Shevchenko V.G., Lupishko D.F. (1998). “Optical properties of Asteroids from Photometric Data.” Solar System Research 32, 220-232.
VizieR (2014). http://vizier.u-strasbg.fr/viz-bin/VizieR.
Warner, B.D. (2016). MPO Software, MPO Canopus v10.7.7.0.
Bdw Publishing. http://minorplanetobserver.com