Stellar kinematics of dwarf galaxies from multi-epoch spectroscopy: application to Triangulum II
We present new MMT/Hectochelle spectroscopic measurements for 257 stars observed along the line of sight to the ultra-faint dwarf galaxy Triangulum II. Combining with results from previous Keck/DEIMOS spectroscopy, we obtain a sample that includes 16 likely members of Triangulum II, with up to 10 in...
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| creator | Buttry, Rachel Pace, Andrew B Koposov, Sergey E Walker, Matthew G Caldwell, Nelson Kirby, Evan N Martin, Nicolas F Mateo, Mario Olszewski, Edward W Starkenburg, Else Badenes, Carles Christine Mazzola Daher |
| description | We present new MMT/Hectochelle spectroscopic measurements for 257 stars observed along the line of sight to the ultra-faint dwarf galaxy Triangulum II. Combining with results from previous Keck/DEIMOS spectroscopy, we obtain a sample that includes 16 likely members of Triangulum II, with up to 10 independent redshift measurements per star. To this multi-epoch kinematic data set we apply methodology that we develop in order to infer binary orbital parameters from sparsely sampled radial velocity curves with as few as two epochs. For a previously-identified (spatially unresolved) binary system in Tri~II, we infer an orbital solution with period \(296.0_{-3.3}^{+3.8} \rm~ days\) , semi-major axis \(1.12^{+0.41}_{-0.24}\rm~AU\), and a systemic velocity \( -380.0 \pm 1.7 \rm~km ~s^{-1}\) that we then use in the analysis of Tri~II's internal kinematics. Despite this improvement in the modeling of binary star systems, the current data remain insufficient to resolve the velocity dispersion of Triangulum II. We instead find a 95% confidence upper limit of \(\sigma_{v} \lesssim 3.4 \rm ~km~s^{-1}\). |
| doi_str_mv | 10.48550/arxiv.2108.10867 |
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Combining with results from previous Keck/DEIMOS spectroscopy, we obtain a sample that includes 16 likely members of Triangulum II, with up to 10 independent redshift measurements per star. To this multi-epoch kinematic data set we apply methodology that we develop in order to infer binary orbital parameters from sparsely sampled radial velocity curves with as few as two epochs. For a previously-identified (spatially unresolved) binary system in Tri~II, we infer an orbital solution with period \(296.0_{-3.3}^{+3.8} \rm~ days\) , semi-major axis \(1.12^{+0.41}_{-0.24}\rm~AU\), and a systemic velocity \( -380.0 \pm 1.7 \rm~km ~s^{-1}\) that we then use in the analysis of Tri~II's internal kinematics. Despite this improvement in the modeling of binary star systems, the current data remain insufficient to resolve the velocity dispersion of Triangulum II. 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We instead find a 95% confidence upper limit of \(\sigma_{v} \lesssim 3.4 \rm ~km~s^{-1}\).</description><subject>Binary stars</subject><subject>Deimos</subject><subject>Dwarf galaxies</subject><subject>Kinematics</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Radial velocity</subject><subject>Red shift</subject><subject>Spectrum analysis</subject><subject>Stellar kinematics</subject><subject>Stellar systems</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotUEFOwzAQtJCQqEofwAlLnFPstZ243FAFNFIlDvQenNQuLk5s7ATa3xNaDqtZaWZHO4PQDSVzLoUg9yoe7PccKJHzcfLiAk2AMZpJDnCFZintCSGQFyAEm6D3t147pyL-tJ1uVW-bhL3B2x8VDd4ppw5WJ2yib3E7uN5mOvjmA6egmz761PhwfMAqBGeb8dh3uPd4E63qdoMbWlyW1-jSKJf07B-naPP8tFmusvXrS7l8XGdKAMuEBM0X2igwzLCmFlKMe06Bk6IGzmnOqdkaagytRS20qZUeKcNrkMVCajZFt2fbU_wqRNuqeKz-aqhONYyKu7MiRP816NRXez_EbvypApFzBkRIxn4B7CxhdQ</recordid><startdate>20220518</startdate><enddate>20220518</enddate><creator>Buttry, Rachel</creator><creator>Pace, Andrew B</creator><creator>Koposov, Sergey E</creator><creator>Walker, Matthew G</creator><creator>Caldwell, Nelson</creator><creator>Kirby, Evan N</creator><creator>Martin, Nicolas F</creator><creator>Mateo, Mario</creator><creator>Olszewski, Edward W</creator><creator>Starkenburg, Else</creator><creator>Badenes, Carles</creator><creator>Christine Mazzola Daher</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>20220518</creationdate><title>Stellar kinematics of dwarf galaxies from multi-epoch spectroscopy: application to Triangulum II</title><author>Buttry, Rachel ; 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Combining with results from previous Keck/DEIMOS spectroscopy, we obtain a sample that includes 16 likely members of Triangulum II, with up to 10 independent redshift measurements per star. To this multi-epoch kinematic data set we apply methodology that we develop in order to infer binary orbital parameters from sparsely sampled radial velocity curves with as few as two epochs. For a previously-identified (spatially unresolved) binary system in Tri~II, we infer an orbital solution with period \(296.0_{-3.3}^{+3.8} \rm~ days\) , semi-major axis \(1.12^{+0.41}_{-0.24}\rm~AU\), and a systemic velocity \( -380.0 \pm 1.7 \rm~km ~s^{-1}\) that we then use in the analysis of Tri~II's internal kinematics. Despite this improvement in the modeling of binary star systems, the current data remain insufficient to resolve the velocity dispersion of Triangulum II. 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| subjects | Binary stars Deimos Dwarf galaxies Kinematics Physics - Astrophysics of Galaxies Radial velocity Red shift Spectrum analysis Stellar kinematics Stellar systems |
| title | Stellar kinematics of dwarf galaxies from multi-epoch spectroscopy: application to Triangulum II |
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