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J/A+A/610/A25       Sulamitis and Clarissa asteroids spectra     (Morate+, 2018)

Visible spectroscopy of the Sulamitis and Clarissa primitive families: a possible link to Erigone and Polana Morate D., de Leon J., De Pra M., Licandro J., Cabrera-Lavers A., Campins H., Pinilla-Alonso N. <Astron. Astrophys. 610, A25 (2018)> =2018A&A...610A..25M (SIMBAD/NED BibCode)
ADC_Keywords: Minor planets ; Solar system ; Spectra, optical Keywords: minor planets, asteroids: general - methods: data analysis - techniques: spectroscopic Abstract: The low-inclination (i<80°) primitive asteroid families in the inner main belt, that is, Polana-Eulalia, Erigone, Sulamitis, and Clarissa, are considered to be the most likely sources of near-Earth asteroids (101955) Bennu and (162173) Ryugu. These two primitive NEAs will be visited by NASA OSIRIS-REx and JAXA Hayabusa 2 missions, respectively, with the aim of collecting samples of material from their surfaces and returning them back to Earth. In this context, the Primitive Asteroid Spectroscopic Survey (PRIMASS) was born, with the main aim to characterize the possible origins of these NEAs and constrain their dynamical evolution. As part of the PRIMASS survey we have already studied the Polana and Erigone collisional families in previously published works. The main goal of the work presented here is to compositionally characterize the Sulamitis and Clarissa families using visible spectroscopy. We have observed 97 asteroids (64 from Sulamitis and 33 from Clarissa) with the OSIRIS instrument (0.5-0.9um) at the 10.4m Gran Telescopio Canarias (GTC). We found that about 60% of the sampled asteroids from the Sulamitis family show signs of aqueous alteration on their surfaces. We also found that the majority of the Clarissa members present no signs of hydration. The results obtained here show similarities between Sulamitis-Erigone, and Clarissa-Polana collisional families. Description: A total of 97 low-resolution visible spectra were obtained for the asteroids in the Sulamitis and Clarissa families (64 and 33 objects, respectively), using the Optical System for Imaging and Low Resolution Integrated Spectroscopy (OSIRIS) camera spectrograph at the 10.4m Gran Telescopio Canarias (GTC), located at the El Roque de los Muchachos Observatory (ORM) in La Palma, Canary Islands, Spain. In addition, we obtained three spectra of (752) Sulamitis using the Intermediate Dispersion Spectrograph (IDS) at the 2.5m Isaac Newton Telescope, also located at the ORM in La Palma, as part of program C97 (2015), on July 22, 2015. All the spectra files included here are named ast_ASTEROIDNUMBER.txt, except for the spectra of (752) taken with the INT (named ast752INT.txt). The first column is the wavelength, expressed in microns, and the second column is the reflectance value (which is normalized at 1 at 0.55 microns). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 68 98 Observational circumstances for the asteroids presented in this work sulamitis/* 40 65 Individual spectra of Sulamitis asteroids clarissa/* 40 33 Individual spectra of Clarissa asteroids
See also: B/astorb : Orbits of Minor Planets (Bowell+ 2014) Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 6 I6 --- Ast Asteroid number 7 A1 --- n_Ast [*] *: Observed with INT 9- 18 A10 "DD-MM-YYYY" Observation date 20- 24 A5 "h:m" Obs.time Observation UT start time 26- 31 A6 s TExp Exposure time 33- 36 F4.1 mag Vmag V magnitude 38- 42 A5 --- SAs ID number of each solar analog star (1) 44- 68 A25 --- FileName Name of the spectrum file
Note (1): Solar analog stars as follows: -------------------------------------------- ID Star RA (J2000) DE Vmag -------------------------------------------- 1 = SA 93-101 01:53:18.0 +00:22:25 9.7 2 = SA 98-978 06:51:34.0 -00:11:28 10.5 3 = SA 102-1081 10:57:04.4 -00:13:10 9.9 4 = SA 107-998 15:38:16.4 +00:15:23 10.4 5 = SA 110-361 18:42:45.0 +00:08:04 12.4 6 = SA 112-1333 20:43:11.8 +00:26:15 10.0 7 = SA 115-271 23:42:41.8 +00:45:10 9.7 --------------------------------------------
Byte-by-byte Description of file: sulamitis/* clarissa/*
Bytes Format Units Label Explanations
4- 16 E13.9 um lambda Wavelength 20- 32 E13.9 --- Refl Relative reflectance (normalized at 1 at 0.55um) 34- 40 F7.5 --- e_Refl ? rms uncertainty on Refl, only for INT spectrum
Acknowledgements: David Morate, damog(at)
(End) Patricia Vannier [CDS] 07-Nov-2017
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