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<ri:Resource created="2011-11-09T14:12:25Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>Spectroscopy of comet C/2004 Q2 (Machholz)</title><shortName>J/ApJ/703/121</shortName><identifier>ivo://CDS.VizieR/J/ApJ/703/121</identifier><altIdentifier>doi:10.26093/cds/vizier.17030121</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Kobayashi H.</name></creator><creator><name>Kawakita H.</name></creator><date role="Updated">2011-11-23T16:55:00Z</date><date role="Created">2011-11-09T14:12:25Z</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>comets</subject><subject>spectroscopy</subject><subject>infrared-astronomy</subject><description>We observed comet C/2004 Q2 (Machholz) with the Keck II telescope in late 2005 January and we obtained the spectra of C/2004 Q2 including many emission lines of volatile species such as H_2_O, HCN, C_2_H_2_, NH_3_, CH_4_, C_2_H_6_, CH_3_OH, and H_2_CO with high-signal-to-noise ratios. Based on our observations, we determined the mixing ratios of the molecules relative to H_2_O in C/2004 Q2. C/2004 Q2 might be the intermediate type between Oort Cloud and Jupiter Family comets. To investigate the formation conditions of such intermediate type comet, we focused on the (C_2_H_2_+C_2_H_6_)/H_2_O ratios and C_2_H_6_/(C_2_H_6_+C_2_H_2_) ratios in comets from the viewpoint of conversion from C_2_H_2_ to C_2_H_6_ in the precometary ices. We employed the dynamical-evolutional model and the chemical-evolutional model to determine the formation region of C/2004 Q2 more precisely. We found that comet C/2004 Q2 might have formed in relatively inner region of the solar nebula than the typical Oort Cloud comet (but slightly further than 5AU from the proto-Sun).</description><source format="bibcode">2009ApJ...703..121K</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/703/121</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>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/169/458">J/ApJS/169/458 : Highly excited H2 in Comets (Liu+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/PAZh/30/946">J/PAZh/30/946 : Unidentified cometary emission lines (Simonia, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/393/1053">J/A+A/393/1053 : 18-cm OH lines in comets (Crovisier+, 2002)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/112/1197">J/AJ/112/1197 : Catalog of cometary emission lines (Brown+ 1996)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/103/83">J/A+AS/103/83 : Line identifications in a fireball spectrum (Borovicka 1994)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/703/121</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/703/121</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/703/121</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/703/121</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/703/121</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/703/121</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface></capability><capability standardID="ivo://ivoa.net/std/TAP#aux"><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://tapvizier.cds.unistra.fr/TAPVizieR/tap</accessURL></interface></capability><coverage><footprint ivo-id="ivo://ivoa.net/std/moc"/><waveband>Infrared</waveband></coverage><tableset><schema><name>default</name><table><name>J/ApJ/703/121/table1</name><description>Line fluxes and g-factors including transmittances</description><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Mol</name><description>Molecule name</description><ucd>meta.id;phys.mol</ucd><dataType xsi:type="vs:VOTableType" arraysize="5*">char</dataType></column><column><name>f_Line</name><description>[a-z ] Indicator of blended line (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>Line</name><description>Line assignment (3)</description><ucd>meta.id;phys.atmol.transition</ucd><dataType xsi:type="vs:VOTableType" arraysize="41*">char</dataType></column><column><name>sigma</name><description>Rest wave number</description><unit>cm**-1</unit><ucd>em.wavenumber</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>FSet1</name><description>? 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