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<ri:Resource created="2017-05-19T15:01:57Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>New SpeX Observations of M7-L6 Dwarfs</title><shortName>J/ApJ/794/143</shortName><identifier>ivo://CDS.VizieR/J/ApJ/794/143</identifier><altIdentifier>doi:10.26093/cds/vizier.17940143</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Bardalez Gagliuffi D.C.</name></creator><creator><name>Burgasser A.J.</name></creator><creator><name>Gelino C.R.</name></creator><creator><name>Looper D.L.,Nicholls C.P.</name></creator><creator><name>Schmidt S.J.</name></creator><creator><name>Cruz K.</name></creator><creator><name>West A.A.</name></creator><creator><name>Gizis J.E.</name></creator><creator><name>Metchev S.</name></creator><date role="Updated">2018-01-23T07:10:53Z</date><date role="Created">2017-05-19T15:01:57Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>dwarf-stars</subject><subject>multiple-stars</subject><subject>stellar-spectral-types</subject><subject>infrared-photometry</subject><description>Multiplicity is a key statistic for understanding the formation of very low mass (VLM) stars and brown dwarfs. Currently, the separation distribution of VLM binaries remains poorly constrained at small separations (&lt;=1 AU), leading to uncertainty in the overall binary fraction. We approach this problem by searching for late-M/early-L plus T dwarf spectral binaries whose combined light spectra exhibit distinct peculiarities, allowing for separation-independent identification. We define a set of spectral indices designed to identify these systems, and we use a spectral template fitting method to confirm and characterize spectral binary candidates from a library of 815 spectra from the SpeX Prism Spectral Libraries. We present 11 new binary candidates, confirm 3 previously reported candidates, and rule out 2 previously identified candidates, all with primary and secondary spectral types in the range M7-L7 and T1-T8, respectively. We find that subdwarfs and blue L dwarfs are the primary contaminants in our sample and propose a method for segregating these sources. If confirmed by follow-up observations, these systems may add to the growing list of tight separation binaries, whose orbital properties may yield further insight into brown dwarf formation scenarios.</description><source format="bibcode">2014ApJ...794..143B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/794/143</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/126/2421">J/AJ/126/2421 : 2MASS-Selected sample of ultracool dwarfs (Cruz+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/2722">J/AJ/131/2722 : New L and T dwarfs from the SDSS (Chiu+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/710/1142">J/ApJ/710/1142 : SpeX spectroscopy of low mass binaries. 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