2023
DOI: 10.1093/pasj/psac109
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Simultaneous multicolor photometry of the DESTINY+ target asteroid (3200) Phaethon

Abstract: Accurate estimations of the brightness of (3200) Phaethon up to lower phase angles are essential for the planning of the on-board camera for the DESTINY+ mission. We carried out intensive observations of Phaethon in the optical wavelength (g, r, and i) with the TriCCS camera on the Seimei 3.8 m telescope in 2021 October and November. We derived the absolute magnitude HV and the slope parameter G of Phaethon as HV = 14.23 ± 0.02 and G = 0.040 ± 0.008 from multiple photometric observations including lower phase … Show more

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Cited by 3 publications
(4 citation statements)
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“…The error-weighted averages of those colors are derived as g − r = 0.714 ± 0.008, r − i = 0.245 ± 0.009, and r − z = 0.255 ± 0.020. The systematic errors in color determination with TriCCS are considered as in Beniyama et al (2023b). The error-weighted average colors correspond to each other within the measurement errors when we consider the results in 2023 January (see Figure 9(b)).…”
Section: Colors and Reflectance Spectrummentioning
confidence: 92%
See 1 more Smart Citation
“…The error-weighted averages of those colors are derived as g − r = 0.714 ± 0.008, r − i = 0.245 ± 0.009, and r − z = 0.255 ± 0.020. The systematic errors in color determination with TriCCS are considered as in Beniyama et al (2023b). The error-weighted average colors correspond to each other within the measurement errors when we consider the results in 2023 January (see Figure 9(b)).…”
Section: Colors and Reflectance Spectrummentioning
confidence: 92%
“…We derived colors and magnitudes of 2015 RN 35 following the procedure described in Beniyama et al (2023aBeniyama et al ( , 2023b Barbary et al 2017). The aperture radii were set to be twice as large as the FWHMs of the point-spread functions of the reference stars in the sidereally stacked images.…”
Section: Seimei Telescopementioning
confidence: 99%
“…The single-exposure time was set to 5.0 s, and the telescope was operated in the nonsidereal tracking mode. The data simultaneously obtained with the g, r, and i or z bands in the Pan-STARRS system (Chambers et al 2016) were analyzed using the same procedure described in Beniyama et al (2023).…”
Section: Photometric Observationsmentioning
confidence: 99%
“…We present the colors of 2010 XC 15 in Figure 4. We estimated the systematic uncertainties of the g − r, r − i, and r − z colors in our observations, δ g−r , δ r−i , and δ r−z , on the basis of the photometric measurements of the reference stars (Beniyama et al 2023): δ g−r = 0.03 and δ r−i = 0.03 in the observations with the g-, r-, and i-band filters on December 23; δ g−r = 0.02 and δ r−z = 0.02 in the observations with the g-, r-, and z-band filters on December 23; δ g−r = 0.02 and δ r−i = 0.02 in the observations with the g-, r-, and i-band filters on December 24; and δ g−r = 0.01 and δ r−z = 0.01 for the observations with the g-, r-, and z-band filters on December 25. The weighted average colors of 2010 XC 15 , except for the first night, when the conditions of the sky were not ideal, were derived as g − r = 0.435 ± 0.008, r − i = 0.158 ± 0.017, and r − z = 0.186 ± 0.009.…”
Section: Colors and Reflectance Spectrummentioning
confidence: 99%