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Optical Spectroscopy and Photometry of Main-Belt Asteroids with a High Orbital Inclination

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Optical Spectroscopy and Photometry of Main-Belt Asteroids with a High Orbital Inclination Home Search Collections Journals About Contact us My IOPscience Optical spectroscopy and photometry of main-belt asteroids with a high orbital inclination This content has been downloaded from IOPscience. Please scroll down to see the full text. 2017 Res. Astron. Astrophys. 17 17 (http://iopscience.iop.org/1674-4527/17/2/17) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 202.52.53.212 This content was downloaded on 24/02/2017 at 08:13 Please note that terms and conditions apply. You may also be interested in: ALBEDO PROPERTIES OF MAIN BELT ASTEROIDS BASED ON THE ALL-SKY SURVEY OF THE INFRARED ASTRONOMICALSATELLITE AKARI Fumihiko Usui, Toshihiro Kasuga, Sunao Hasegawa et al. WISE/NEOWISE OBSERVATIONS OF THE JOVIAN TROJAN POPULATION: TAXONOMY T. Grav, A. K. Mainzer, J. M. Bauer et al. CAPTURE OF TRANS-NEPTUNIAN PLANETESIMALS IN THE MAIN ASTEROID BELT David Vokrouhlický, William F. Bottke and David Nesvorný HIGH ECLIPTIC LATITUDE SURVEY FOR SMALL MAIN-BELT ASTEROIDS Tsuyoshi Terai, Jun Takahashi and Yoichi Itoh Solar System Objects in the SDSS Željko Ivezi, Serge Tabachnik, Roman Rafikov et al. NEOWISE STUDIES OF SPECTROPHOTOMETRICALLY CLASSIFIED ASTEROIDS: PRELIMINARY RESULTSA. Mainzer, T. Grav, J. Masiero et al. MAIN-BELT ASTEROIDS WITH WISE/NEOWISE: NEAR-INFRARED ALBEDOS Joseph R. Masiero, T. Grav, A. K. Mainzer et al. AKARI/AcuA PHYSICAL STUDIES OF THE CYBELE ASTEROID FAMILY Toshihiro Kasuga, Fumihiko Usui, Sunao Hasegawa et al. MULTIPLE AND FAST: THE ACCRETION OF ORDINARY CHONDRITE PARENT BODIES P. Vernazza, B. Zanda, R. P. Binzel et al. RAA 2017 Vol. 17 No. 2, 17 (8pp) doi: 10.1088/1674–4527/17/2/17 R c 2017 National Astronomical Observatories, CAS and IOP Publishing Ltd. esearch in Astronomy and http://www.raa-journal.org http://iopscience.iop.org/raa Astrophysics Optical spectroscopy and photometry of main-belt asteroids with a high orbital inclination Aya Iwai1, Yoichi Itoh2, Tsuyoshi Terai3, Ranjan Gupta4, Asoke Sen5 and Jun Takahashi2 1 National Institute of Advanced Industrial Science and Technology, Ibaraki 305-8563, Japan 2 Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, Hyogo 679-5313, Japan; [email protected] 3 National Astronomical Observatory of Japan, Hilo, Hawaii 96720, USA 4 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411 007, India 5 Department of Physics, Assam University, Silchar 788 001, India Received 2016 August 9; accepted 2016 October 24 Abstract We carried out low-resolution optical spectroscopy of 51 main-belt asteroids, most of which have highly-inclined orbits. They are selected from D-type candidates in the SDSS-MOC 4 catalog. Using the University of Hawaii 2.2 m telescope and the Inter-University Centre for Astronomy and Astrophysics 2m telescope in India, we determined the spectral types of 38 asteroids. Among them, eight asteroids were classified as D-type asteroids. Fractions of D-type asteroids are 3.0 ± 1.1% for low orbital inclination main-belt asteroids and 7.3 ± 2.0% for high orbital inclination main-belt asteroids. The results of our study indicate that some D-type asteroids were formed within the ecliptic region between the main belt and Jupiter, and were then perturbed by Jupiter. Key words: minor planets, asteroids: general — techniques: spectroscopic 1 INTRODUCTION the origin of high orbital inclination asteroids is still un- certain. Nagasawa et al. (2000) simulated the orbital evo- Asteroids with a high orbital inclination are outliers. lution of asteroids. They included the depletion of gas in Terai & Itoh (2011) surveyed small asteroids at high the solar nebula. An inner edge of the gas was moving ecliptic latitudes. By using wide and deep optical im- outward at a velocity of 1 × 10−5 AU yr−1. Their study ages taken with Suprime-Cam mounted on the Subaru revealed that the eccentricity and inclination of the aster- Telescope, they detected 656 asteroids with high orbital oids increased due to the motion of secular resonances inclinations. The orbital semi-major axes of most of these caused by gas depletion, but the semi-major axis of the asteroids were derived to be between 2.0 astronomical asteroids did not change. Ida & Makino (1993) investi- units (AU) and 3.3AU. Terai et al. (2013) found that gated the orbital evolution of planetesimals near a pro- the cumulative size distribution of high orbital inclina- toplanet. Their numerical simulations showed that the tion main-belt asteroids (hereafter MBAs) was shallower planetesimals moved inward or outward with increasing than that of low orbital inclination MBAs. It is generally orbital inclinations and/or eccentricities due to the gravi- believed that MBAs with high orbital inclinations have tational perturbation of a protoplanet. high collisional velocities. The shallow size distribution In this paper, we focus on D-type asteroids. D-type for high orbital inclination MBAs indicates that a large asteroids are abundant in the Trojan and main-belt popu- body has a higher disruptive strength when hyperveloc- lation with a semi-major axis beyond ≃3AU. Optical re- ity impacts occur. flectance of D-type asteroids increases significantly with The size distribution of high orbital inclination aster- wavelength. Such optical reflectance and low albedo of oids provides us with information regarding the process D-type asteroids are similar to those of some comet nu- of planetesimal collision under different conditions com- clei. Many properties of D-type asteroids, including their pared to low orbital inclination planetesimals. However, spatial distribution and optical reflectance, have been dis- 17–2 A. Iwai et al.: Highly-Inclined Asteroids cussed in the context of cometary evolution and asteroid tion greater than 10◦. We selected high orbital inclination populations. Detailed discussions on D-type asteroids are asteroids because of the lack of high inclination samples found, e.g., in Fitzsimmons et al. (1994). in previous studies. One may postulate that the defini- We acquired low-resolution optical spectroscopy of tion of high and low orbital inclination asteroids should MBAs. Most of these asteroids have highly-inclined or- be based on the ν6 resonance. Because the orbital incli- bits and optical colors consistent with spectral type D. nation of the ν6 resonance varies with semi-major axis, A comparison of the number ratio for D-type asteroids classification based on the ν6 resonance may complicate in high and low inclination populations will help us to the discussion on the selection bias of targets. Instead, understand the formation and evolution process of high we simply define high and low orbital inclination aster- inclination asteroids. However, we cannot directly ap- oids based on their inclinations. Most of the selected as- ply the D-type ratio from large volume photometric cata- teroids are listed in the SDSS-MOC 4 catalog and their logs, e.g., the Sloan Digital Sky Survey - Moving Object optical magnitudes are given. We constructed an opti- Catalog 4 (SDSS-MOC 4) catalog, because classifica- cal color-color diagram of the selected asteroids using tion using multi-color photometry is not certain (Carvano the SDSS magnitudes, and classified those objects with et al. 2010, DeMeo & Carry 2013, DeMeo & Carry g−r ≥ 0.5 mag and r−i ≥ 0.2 mag as candidates for D- 2014). Therefore, we carried out spectroscopic observa- type asteroids (Ivezi´cet al. 2001). Because we selected tions confirming D-type candidates and estimating the the targets on the gri color-color diagram, we also con- real D-type ratio. Hereafter, we define low orbital in- sidered the selection bias arising from the gri color-color clination MBAs as asteroids with a semi-major axis be- diagram (Sect. 4). tween 2.1AU and 3.3AU and with inclinations less than We were not able to completely fill the observing ◦ 10 , and high orbital inclination MBAs as asteroids with time while searching for D-type asteroids. Therefore, the same semi-major axis range but with inclinations when we could not find any suitable candidates, we ob- ◦ equal to or larger than 10 . served high orbital inclination asteroids instead, even if their SDSS colors were unknown. As a result, we ob- 2 OBSERVATIONS served a total of 48 high orbital inclination asteroids. We We carried out low-resolution optical spectroscopy of also observed three low orbital inclination asteroids for MBAs using the Wide Field Grism Spectrograph 2 reference. The optical spectra of dwarfs with a spectral (WFGS2) mounted on the University of Hawaii (UH) type of G were also taken as spectral standards. 2.2m telescope. The data were obtainedon 2008 October After the observations for this work were carried out, 30 and 31 and 2011 October 19 and 20 with the low- DeMeo & Carry (2013) proposed a new method for the dispersion grism 1 and a 1.4′′ width slit. These instru- related taxonomy by using SDSS g-, r-, i- and z-band ment settings achieved a wavelength coverage of 440– filters. They claimed that asteroid types can be identified 830nm and a spectral resolution of ∼410 at 650nm. Slit with the gri slope and i − z color. D-type asteroids are orientations were fixed in the north-south direction. The classified as the group with the reddest gri slope and the telescope was operated in non-sidereal tracking mode. reddest i − z color. The targets in this paper were classi- The integration time for each object was between 180s fied into D-type, L-type or S-type with large i−z magni- and 600s. Facilities managed by the Inter-University tudes by applying the classification system of DeMeo & Centre for Astronomy and Astrophysics (IUCAA) were Carry (2013). Efficiency in the discovery of D-type aster- also used. We employed the IUCAA Faint Object oids would increase if we used the classification method Spectrograph and Camera (IFOSC) mounted on the 2m of DeMeo & Carry (2013).
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