Intermediate resolution near-infrared spectroscopy of 36 late M dwarfs

Intermediate resolution near-infrared
spectroscopy of 36 late M dwarfs
Deshpande R., Martin E.L., Montgomery M.M., Zapatero
Osorio M.R., Rodler F., Del Burgo C., Phan Bao N., Lyubchik
Y., Tata R., Bouy H., Pavlenko Y.
Center for Exoplanets and Habitable Worlds, Pennsylvania State
University, University Park, PA 16802, United States; Department of
Astronomy and Astrophysics, Pennsylvania State University,
University Park, PA 16802, United States; Department of Physics,
University of Central Florida, P.O. Box 162385, Orlando, FL 328162385, United States; Centro de Astrobiología (CSIC-INTA), Ctra.
Ajalvir km 4, E-28850 Torrejón de Ardoz, Madrid, Spain; Institut de
Ciencies de l'Espai (CSIC-IEEC), Campus UAB, Torre C5-parell-2a
planta, E-08193 Bellaterra, Spain; Instituto de Astrofísica de
Canarias, c/Vía Láctea s/n, E-38205 La Laguna, Islas Canarias,
Tenerife, Spain; Instituto Nacional de Astrofísica, Óptica y
Electrónica (INAOE), Aptdo. Postal 51 y 216, Pue., 72000 Puebla,
Mexico; UNINOVA-CA3, Campus da Caparica, Quinta da Torre,
2825-149 Caparica, Monte de Caparica, Portugal; Department of
Physics, HCMIU, HCM Vietnam National University, Thu Duc
District, Viet Nam; Institute of Astronomy and Astrophysics, Academia
Sinica, P.O. Box 23-141, Taipei 106, Taiwan; Main Astronomical
Observatory of Academy of Sciences of Ukraine, Zabolotnoho 27, Kyiv
03680, Ukraine
Abstract: We present observations of 36 late M dwarfs obtained with the Keck
II/NIRSPEC in the J band at a resolution of ∼20,000. We have measured
projected rotational velocities, absolute radial velocities, and pseudo-equivalent
widths of atomic lines. Twelve of our targets did not have previous
measurements in the literature. For the other 24 targets, we confirm previously
reported measurements. We find that 13 stars from our sample have v sin i below
our measurement threshold (12kms -1) whereas four of our targets are fast
rotators (v sin i > 30kms -1). As fast rotation causes spectral features to be
washed out, stars with low projected rotational velocities are sought for radial
velocity surveys. At our intermediate spectral resolution, we have confirmed the
identification of neutral atomic lines reported in McLean etal. We also calculated
pseudo-equivalent widths of 12 atomic lines. Our results confirm that the
pseudo-equivalent width of K I lines is strongly dependent on spectral types. We
observe that the pseudo-equivalent width of Fe I and Mn I lines remains fairly
constant with later spectral type. We suggest that these lines are particularly
suitable for deriving metallicities for late M dwarfs. © 2012. The American
Astronomical Society. All rights reserved.
Author Keywords: brown dwarfs; planetary systems; stars: fundamental
parameters; stars: low-mass; stars: rotation; techniques: radial velocities
Year: 2012
Source tilte: Astronomical Journal
Volume: 144
Page: Link: http://www.scopus.com/inward/record.url?eid=2-s2.084866348674&partnerID=40&md5=8420b745a758424b257907a41fc01e28
Correspondence Address: Deshpande, R.; Center for Exoplanets and Habitable
Worlds, Pennsylvania State University, University Park, PA 16802, United
States; email: [email protected]
Editors:
ISSN: 46256
ISBN:
DOI: 10.1088/0004-6256/144/4/99
Language of Original Document: English
Abbreviated Source Title: Astron. J.
Document Type: Article
Source: Scopus
Authors with affiliations:
Deshpande, R., Center for Exoplanets and Habitable Worlds, Pennsylvania State
University, University Park, PA 16802, United States, Department of Astronomy
and Astrophysics, Pennsylvania State University, University Park, PA 16802,
United States, Department of Physics, University of Central Florida, P.O. Box
162385, Orlando, FL 32816-2385, United States; Martín, E.L., Centro de
Astrobiología (CSIC-INTA), Ctra. Ajalvir km 4, E-28850 Torrejón de Ardoz,
Madrid, Spain; Montgomery, M.M., Department of Physics, University of
Central Florida, P.O. Box 162385, Orlando, FL 32816-2385, United States;
Zapatero Osorio, M.R., Centro de Astrobiología (CSIC-INTA), Ctra. Ajalvir km
4, E-28850 Torrejón de Ardoz, Madrid, Spain; Rodler, F., Institut de Ciencies de
l'Espai (CSIC-IEEC), Campus UAB, Torre C5-parell-2a planta, E-08193
Bellaterra, Spain, Instituto de Astrofísica de Canarias, c/Vía Láctea s/n, E-38205
La Laguna, Islas Canarias, Tenerife, Spain; Del Burgo, C., Instituto Nacional de
Astrofísica, Óptica y Electrónica (INAOE), Aptdo. Postal 51 y 216, Pue., 72000
Puebla, Mexico, UNINOVA-CA3, Campus da Caparica, Quinta da Torre, 2825149 Caparica, Monte de Caparica, Portugal; Phan Bao, N., Department of
Physics, HCMIU, HCM Vietnam National University, Thu Duc District, Viet
Nam, Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23141, Taipei 106, Taiwan; Lyubchik, Y., Main Astronomical Observatory of
Academy of Sciences of Ukraine, Zabolotnoho 27, Kyiv 03680, Ukraine; Tata,
R., Instituto de Astrofísica de Canarias, c/Vía Láctea s/n, E-38205 La Laguna,
Islas Canarias, Tenerife, Spain; Bouy, H., Centro de Astrobiología (CSICINTA), Ctra. Ajalvir km 4, E-28850 Torrejón de Ardoz, Madrid, Spain;
Pavlenko, Y., Main Astronomical Observatory of Academy of Sciences of
Ukraine, Zabolotnoho 27, Kyiv 03680, Ukraine

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