IRTF Data Archive Program Information

# # Program information file # PROGRAM_ID 2021A067 PROGRAM_TITLE Hungaria Asteroid Region Telescopic Spectral Survey [HARTSS]: Mineralogy and Taxonomy of Hungaria Family Members PROGRAM_INV1 Michael Lucas PROGRAM_INV2 Richard Cartwright PROGRAM_INV3 Josh Emery PROGRAM_INV4 PROGRAM_INV5 PROGRAM_SCICAT solar system PROGRAM_ABSTRACT_BEG We propose near-infrared [NIR] spectroscopy with the SpeX instrument in prism mode at the IRTF for 16 small asteroids [D~2.9 to 1.4 km; Hv = 14.0 to 5.5] that belong to the Hungaria collisional family to determine whether the fragments of this family are compositionally homogeneous, or conversely heterogeneous. We will search for Hungaria family asteroids that exhibit NIR absorption features centered around ~0.9 um, which are attributed to iron-poor orthopyroxene [i.e., enstatite], and/or the sulfide mineral oldhamite [Ca,Mg]S. We will also determine if these Hungaria family members are consistent with Bus-DeMeo taxonomic Xe-type, which is the classification of the largest collisional fragment and family namesake 434 Hungaria [D~11 km], and several other large family members observed during our on-going spectral survey of Hungaria asteroids [HARTSS]. Xe-type asteroids have average albedo of pv=0.536, therefore Hungaria family members in the Hv ~14.0-15.5 range have estimated diameters between 2.9 to 1.4 km respectively, and provide a sample of small Hungaria family fragments as a basis for spectral analysis and comparison. Combined with previous observations of 24 Hungaria family members obtained using SpeX, these new observations will represent the most thorough examination yet of the spectral and mineralogical features of Hungaria family members. We require S/N ~100 over the wavelength range of 0.65-2.5 um to detect weak absorption features due to enstatite and/or the sulfide mineral oldhamite. SpeX in low-resolution prism mode can acquire spectra of sufficient quality to accurately characterize these absorption features for asteroids with Vmag of ~16.5 to 17.2 using integration times of 32 to 80 minutes. Therefore, we can observe all 16 asteroids within two full-night observing runs in IRTF semester 2021A. PROGRAM_ABSTRACT_END