Characterizing K2 Candidate Planetary Systems Orbiting Low-Mass Stars IV: Updated Properties for 86 Cool Dwarfs Observed During Campaigns 1-17
We present revised stellar properties for 172 K2 target stars that were identified as possible hosts of transiting planets during Campaigns 1-17. Using medium-resolution near-infrared spectra acquired with the NASA Infrared Telescope Facility/SpeX and Palomar/TripleSpec, we found that 86 of our targ...
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| creator | Dressing, Courtney D Hardegree-Ullman, Kevin Schlieder, Joshua E Newton, Elisabeth Vanderburg, Andrew Feinstein, Adina D Duvvuri, Girish M Arnold, Lauren Bristow, Makennah Thackeray, Beverly Ellianna Schwab Abrahams Ciardi, David Crossfield, Ian Yu, Liang Martinez, Arturo O Christiansen, Jessie L Crepp, Justin R Isaacson, Howard |
| description | We present revised stellar properties for 172 K2 target stars that were identified as possible hosts of transiting planets during Campaigns 1-17. Using medium-resolution near-infrared spectra acquired with the NASA Infrared Telescope Facility/SpeX and Palomar/TripleSpec, we found that 86 of our targets were bona fide cool dwarfs, 74 were hotter dwarfs, and 12 were giants. Combining our spectroscopic metallicities with Gaia parallaxes and archival photometry, we derived photometric stellar parameters and compared them to our spectroscopic estimates. Although our spectroscopic and photometric radius and temperature estimates are consistent, our photometric mass estimates are systematically 0.11 solar masses (34%) higher than our spectroscopic mass estimates for the least massive stars (photometric mass estimates < 0.4 solar masses). Adopting the photometric parameters and comparing our results to parameters reported in the Ecliptic Plane Input Catalog, our revised stellar radii are 0.15 solar radii (40%) larger and our revised stellar effective temperatures are roughly 65K cooler. Correctly determining the properties of K2 target stars is essential for characterizing any associated planet candidates, estimating the planet search sensitivity, and calculating planet occurrence rates. Even though Gaia parallaxes have increased the power of photometric surveys, spectroscopic characterization remains essential for determining stellar metallicities and investigating correlations between stellar metallicity and planetary properties. |
| doi_str_mv | 10.48550/arxiv.1905.11457 |
| format | Article |
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Using medium-resolution near-infrared spectra acquired with the NASA Infrared Telescope Facility/SpeX and Palomar/TripleSpec, we found that 86 of our targets were bona fide cool dwarfs, 74 were hotter dwarfs, and 12 were giants. Combining our spectroscopic metallicities with Gaia parallaxes and archival photometry, we derived photometric stellar parameters and compared them to our spectroscopic estimates. Although our spectroscopic and photometric radius and temperature estimates are consistent, our photometric mass estimates are systematically 0.11 solar masses (34%) higher than our spectroscopic mass estimates for the least massive stars (photometric mass estimates < 0.4 solar masses). Adopting the photometric parameters and comparing our results to parameters reported in the Ecliptic Plane Input Catalog, our revised stellar radii are 0.15 solar radii (40%) larger and our revised stellar effective temperatures are roughly 65K cooler. Correctly determining the properties of K2 target stars is essential for characterizing any associated planet candidates, estimating the planet search sensitivity, and calculating planet occurrence rates. Even though Gaia parallaxes have increased the power of photometric surveys, spectroscopic characterization remains essential for determining stellar metallicities and investigating correlations between stellar metallicity and planetary properties.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1905.11457</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Estimates ; Extrasolar planets ; Infrared spectra ; Infrared telescopes ; Low mass stars ; Massive stars ; Metallicity ; Near infrared radiation ; Parameters ; Photometry ; Physics - Earth and Planetary Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planetary systems ; Properties (attributes) ; Spectroscopy ; Stellar mass ; Target recognition ; Transit</subject><ispartof>arXiv.org, 2019-05</ispartof><rights>2019. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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Correctly determining the properties of K2 target stars is essential for characterizing any associated planet candidates, estimating the planet search sensitivity, and calculating planet occurrence rates. Even though Gaia parallaxes have increased the power of photometric surveys, spectroscopic characterization remains essential for determining stellar metallicities and investigating correlations between stellar metallicity and planetary properties.</description><subject>Estimates</subject><subject>Extrasolar planets</subject><subject>Infrared spectra</subject><subject>Infrared telescopes</subject><subject>Low mass stars</subject><subject>Massive stars</subject><subject>Metallicity</subject><subject>Near infrared radiation</subject><subject>Parameters</subject><subject>Photometry</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planetary systems</subject><subject>Properties (attributes)</subject><subject>Spectroscopy</subject><subject>Stellar mass</subject><subject>Target recognition</subject><subject>Transit</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkE1PwkAQhjcmJhLkB3hyE8_F_WyLN1O_iBhIQK_NtJ3FJdDW3QLij_A324KnOczzvpl5CLnibKhirdktuG-7G_IR00POlY7OSE9IyYNYCXFBBt6vGGMijITWskd-k09wkDfo7I8tl_RV0ATKwhbQIJ2tocQG3IHOD77BjadTl9mm4ybVPngD7-m83Xs6_rij73UXKujMVTW6xqKnpnI0DmlSVWv6sAdn2obMo9u12MPWdUUJbGqwy9JTHvDokpwbWHsc_M8-WTw9LpKXYDJ9Hif3kwC0UEEoCwGIRR4Wkhlkho0kKolMRihz5CaMjTQGioKzEWSM6UzloLJWh-IRGtkn16fao6y0dnbTfpl20tKjtJa4ORG1q7626Jt0VW1d2d6UCiF52DJMyT-MkXA4</recordid><startdate>20190527</startdate><enddate>20190527</enddate><creator>Dressing, Courtney D</creator><creator>Hardegree-Ullman, Kevin</creator><creator>Schlieder, Joshua E</creator><creator>Newton, Elisabeth</creator><creator>Vanderburg, Andrew</creator><creator>Feinstein, Adina D</creator><creator>Duvvuri, Girish M</creator><creator>Arnold, Lauren</creator><creator>Bristow, Makennah</creator><creator>Thackeray, Beverly</creator><creator>Ellianna Schwab Abrahams</creator><creator>Ciardi, David</creator><creator>Crossfield, Ian</creator><creator>Yu, Liang</creator><creator>Martinez, Arturo O</creator><creator>Christiansen, Jessie L</creator><creator>Crepp, Justin R</creator><creator>Isaacson, Howard</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20190527</creationdate><title>Characterizing K2 Candidate Planetary Systems Orbiting Low-Mass Stars IV: Updated Properties for 86 Cool Dwarfs Observed During Campaigns 1-17</title><author>Dressing, Courtney D ; Hardegree-Ullman, Kevin ; Schlieder, Joshua E ; Newton, Elisabeth ; Vanderburg, Andrew ; Feinstein, Adina D ; Duvvuri, Girish M ; Arnold, Lauren ; Bristow, Makennah ; Thackeray, Beverly ; Ellianna Schwab Abrahams ; Ciardi, David ; Crossfield, Ian ; Yu, Liang ; Martinez, Arturo O ; Christiansen, Jessie L ; Crepp, Justin R ; Isaacson, Howard</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a524-63d2aeedc6d30fe0f093e43e037e3ce1f68f3ffadd109ab005b4ca4b145417ef3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Estimates</topic><topic>Extrasolar planets</topic><topic>Infrared spectra</topic><topic>Infrared telescopes</topic><topic>Low mass stars</topic><topic>Massive stars</topic><topic>Metallicity</topic><topic>Near infrared radiation</topic><topic>Parameters</topic><topic>Photometry</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Planetary systems</topic><topic>Properties (attributes)</topic><topic>Spectroscopy</topic><topic>Stellar mass</topic><topic>Target recognition</topic><topic>Transit</topic><toplevel>online_resources</toplevel><creatorcontrib>Dressing, Courtney D</creatorcontrib><creatorcontrib>Hardegree-Ullman, Kevin</creatorcontrib><creatorcontrib>Schlieder, Joshua E</creatorcontrib><creatorcontrib>Newton, Elisabeth</creatorcontrib><creatorcontrib>Vanderburg, Andrew</creatorcontrib><creatorcontrib>Feinstein, Adina D</creatorcontrib><creatorcontrib>Duvvuri, Girish M</creatorcontrib><creatorcontrib>Arnold, Lauren</creatorcontrib><creatorcontrib>Bristow, Makennah</creatorcontrib><creatorcontrib>Thackeray, Beverly</creatorcontrib><creatorcontrib>Ellianna Schwab Abrahams</creatorcontrib><creatorcontrib>Ciardi, David</creatorcontrib><creatorcontrib>Crossfield, Ian</creatorcontrib><creatorcontrib>Yu, Liang</creatorcontrib><creatorcontrib>Martinez, Arturo O</creatorcontrib><creatorcontrib>Christiansen, Jessie L</creatorcontrib><creatorcontrib>Crepp, Justin R</creatorcontrib><creatorcontrib>Isaacson, Howard</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Dressing, Courtney D</au><au>Hardegree-Ullman, Kevin</au><au>Schlieder, Joshua E</au><au>Newton, Elisabeth</au><au>Vanderburg, Andrew</au><au>Feinstein, Adina D</au><au>Duvvuri, Girish M</au><au>Arnold, Lauren</au><au>Bristow, Makennah</au><au>Thackeray, Beverly</au><au>Ellianna Schwab Abrahams</au><au>Ciardi, David</au><au>Crossfield, Ian</au><au>Yu, Liang</au><au>Martinez, Arturo O</au><au>Christiansen, Jessie L</au><au>Crepp, Justin R</au><au>Isaacson, Howard</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Characterizing K2 Candidate Planetary Systems Orbiting Low-Mass Stars IV: Updated Properties for 86 Cool Dwarfs Observed During Campaigns 1-17</atitle><jtitle>arXiv.org</jtitle><date>2019-05-27</date><risdate>2019</risdate><eissn>2331-8422</eissn><abstract>We present revised stellar properties for 172 K2 target stars that were identified as possible hosts of transiting planets during Campaigns 1-17. Using medium-resolution near-infrared spectra acquired with the NASA Infrared Telescope Facility/SpeX and Palomar/TripleSpec, we found that 86 of our targets were bona fide cool dwarfs, 74 were hotter dwarfs, and 12 were giants. Combining our spectroscopic metallicities with Gaia parallaxes and archival photometry, we derived photometric stellar parameters and compared them to our spectroscopic estimates. Although our spectroscopic and photometric radius and temperature estimates are consistent, our photometric mass estimates are systematically 0.11 solar masses (34%) higher than our spectroscopic mass estimates for the least massive stars (photometric mass estimates < 0.4 solar masses). Adopting the photometric parameters and comparing our results to parameters reported in the Ecliptic Plane Input Catalog, our revised stellar radii are 0.15 solar radii (40%) larger and our revised stellar effective temperatures are roughly 65K cooler. Correctly determining the properties of K2 target stars is essential for characterizing any associated planet candidates, estimating the planet search sensitivity, and calculating planet occurrence rates. Even though Gaia parallaxes have increased the power of photometric surveys, spectroscopic characterization remains essential for determining stellar metallicities and investigating correlations between stellar metallicity and planetary properties.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1905.11457</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Estimates Extrasolar planets Infrared spectra Infrared telescopes Low mass stars Massive stars Metallicity Near infrared radiation Parameters Photometry Physics - Earth and Planetary Astrophysics Physics - Solar and Stellar Astrophysics Planetary systems Properties (attributes) Spectroscopy Stellar mass Target recognition Transit |
| title | Characterizing K2 Candidate Planetary Systems Orbiting Low-Mass Stars IV: Updated Properties for 86 Cool Dwarfs Observed During Campaigns 1-17 |
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