ESASky SSOSS: Solar System Object Search Service and the case of Psyche

<div class="">Asteroids reflectance spectra in the visible light will be one of the novel products of the Gaia Data Release 3 (DR3). These spectra are produced from Gaia observations obtained by means of the blue and red photometers &#8212; the so-called BP and RP, respectively. We will review the strategy adopted to produce asteroid reflectance spectra from BP-RP data, focusing on the choice of spectro-photometric calibrations computed taking into account solar system object astrometry and suitable lists of solar-analog stars.</div> <div class="">&#160;</div> <div class="">Our preliminary investigation shows that we will be able to obtain reflectance spectra for asteroids as small as some km in the main belt, by exploiting the fact that each object has been observed multiple times by Gaia. We will show the capability of Gaia to probe the detailed compositional gradient of the main belt down to small sizes and to study correlations between spectral classes and other asteroid physical parameters, such as albedo and size.</div> <div class="">&#160;</div> <div class="">Concerning the brightest asteroids, we expect to have substantial signal at wavelengths shorter than 450 nm, allowing Gaia to examine this region of the spectrum that has been poorly investigated by ground-based asteroid spectroscopic surveys. This region is characterised by the presence of a reflectance downturn that is diagnostic for the composition of classes of primitive asteroids, for instance those including the parent bodies of carbonaceous chondrites. These asteroids may have played an important role for the delivery of prebiotic compounds to Earth during the early phases of solar system' s history and, as such, are at the center of attention of the planetary science community.&#160;</div>

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Simultaneous visible and near-infrared time resolved observations of the outer Solar System object (29981) 1999 TD10

Icarus ◽

10.1016/j.icarus.2004.05.021 ◽

2004 ◽

Vol 171 (2) ◽

pp. 506-515 ◽

Cited By ~ 10

Author(s):

Béatrice E.A. Mueller ◽

Carl W. Hergenrother ◽

Nalin H. Samarasinha ◽

Humberto Campins ◽

Donald W. McCarthy

Keyword(s):

Solar System ◽

Near Infrared ◽

Outer Solar System ◽

Time Resolved ◽

Solar System Object

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A portrait of the extreme solar system object 2012 DR30

Astronomy and Astrophysics ◽

10.1051/0004-6361/201321147 ◽

2013 ◽

Vol 555 ◽

pp. A3 ◽

Cited By ~ 11

Author(s):

Cs. Kiss ◽

Gy. Szabó ◽

J. Horner ◽

B. C. Conn ◽

T. G. Müller ◽

...

Keyword(s):

Solar System ◽

Solar System Object

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Solar System Object Image Search: A precovery search engine

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315008704 ◽

2015 ◽

Vol 10 (S318) ◽

pp. 270-273

Author(s):

Stephen D. J. Gwyn ◽

Norman Hill ◽

JJ Kavelaars

Keyword(s):

Solar System ◽

Moving Objects ◽

Object Image ◽

Image Search ◽

Moving Targets ◽

Orbital Elements ◽

Data Centre ◽

Astronomical Image ◽

Solar System Object ◽

The Web

AbstractWhile regular astronomical image archive searches can find images at a fixed location, they cannot find images of moving targets such as asteroids or comets. The Solar System Object Image Search (SSOIS) at the Canadian Astronomy Data Centre allows users to search for images of moving objects, allowing precoveries. SSOIS accepts as input either an object designation, a list of observations, a set of orbital elements, or a user-generated ephemeris for an object. It then searches for observations of that object over a range of dates. The user is then presented with a list of images containing that object from a variety of archives. Initially created to search the CFHT MegaCam archive, SSOIS has been extended to other telescopes including Gemini, Subaru/SuprimeCam, WISE, HST, the SDSS, AAT, the ING telescopes, the ESO telescopes, and the NOAO telescopes (KPNO/CTIO/WIYN), for a total of 24.5 million images. As the Pan-STARRS and Hyper Suprime-Cam archives become available, they will be incorporated as well. The SSOIS tool is located on the web at http://www.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/en/ssois/.

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An Efficient Astronomical Image Representation for Solar System Object Searches

Publications of the Astronomical Society of the Pacific ◽

10.1086/674695 ◽

2014 ◽

Vol 126 (935) ◽

pp. 70-78 ◽

Cited By ~ 2

Author(s):

David L. Clark

Keyword(s):

Solar System ◽

Image Representation ◽

Astronomical Image ◽

Solar System Object

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The Atacama Cosmology Telescope: A Search for Planet 9

The Astrophysical Journal ◽

10.3847/1538-4357/ac2307 ◽

2021 ◽

Vol 923 (2) ◽

pp. 224

Author(s):

Sigurd Naess ◽

Simone Aiola ◽

Nick Battaglia ◽

Richard J. Bond ◽

Erminia Calabrese ◽

...

Keyword(s):

Detection Limit ◽

Solar System ◽

Angular Velocity ◽

Flux Density ◽

Millimeter Wave ◽

Survey Area ◽

Atacama Cosmology Telescope ◽

Solar System Object ◽

Wave Flux

Abstract We use Atacama Cosmology Telescope (ACT) observations at 98 GHz (2015–2019), 150 GHz (2013–2019), and 229 GHz (2017–2019) to perform a blind shift-and-stack search for Planet 9. The search explores distances from 300 au to 2000 au and velocities up to 6.′3 per year, depending on the distance (r). For a 5 Earth-mass Planet 9 the detection limit varies from 325 au to 625 au, depending on the sky location. For a 10 Earth-mass planet the corresponding range is 425 au to 775 au. The predicted aphelion and most likely location of the planet corresponds to the shallower end of these ranges. The search covers the whole 18,000 square degrees of the ACT survey. No significant detections are found, which is used to place limits on the millimeter-wave flux density of Planet 9 over much of its orbit. Overall we eliminate roughly 17% and 9% of the parameter space for a 5 and 10 Earth-mass Planet 9, respectively. These bounds approach those of a recent INPOP19a ephemeris-based analysis, but do not exceed it. We also provide a list of the 10 strongest candidates from the search for possible follow-up. More generally, we exclude (at 95% confidence) the presence of an unknown solar system object within our survey area brighter than 4–12 mJy (depending on position) at 150 GHz with current distance 300 au < r < 600 au and heliocentric angular velocity 1 .′ 5 yr − 1 < v · 500 au r < 2 .″ 3 yr − 1 , corresponding to low-to-moderate eccentricities. These limits worsen gradually beyond 600 au, reaching 5–15 mJy by 1500 au.

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