CARMENES: high-resolution spectra and precise radial velocities in the red and infrared
CARMENES: high-resolution spectra and precise radial velocities in the red and infrared
复制标题
CARMENES：红色和红外的高分辨率光谱和精确的径向速度
DOI：
--
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发表时间：
2018
期刊：
影响因子：
--
通讯作者：
Z. Zhao
中科院分区：
文献类型：
--
作者：
A. Quirrenbach;P. Amado;I. Ribas;A. Reiners;J. Caballero;W. Seifert;J. Aceituno;M. Azzaro;D. Baroch;D. Barrado;F. Bauer;F. Bauer;S. Becerril;V. Béjar;D. Benítez;M. Brinkmöller;C. Guillén;C. Cifuentes;J. Colomé;M. Cortés;S. Czesla;S. Dreizler;K. Frölich;B. Fuhrmeister;D. Galadí;J. Hernández;R. Peinado;E. Guenther;E. D. Guindos;H. Hagen;A. Hatzes;P. Hauschildt;J. Helmling;T. Henning;O. Herbort;L. Castano;E. Herrero;D. Hintz;S. Jeffers;E. Johnson;E. D. Juan;A. Kaminski;H. Klahr;M. Kürster;M. Lafarga;L. Sairam;M. Lampón;L. Lara;R. Launhardt;M. Fresno;M. López‐Puertas;R. Luque;H. Mandel;E. Marfil;E. Martín;S. Martín;Richard J. Mathar;D. Montes;J. Morales;E. Nagel;L. Nortmann;G. Nowak;E. Pallé;V. Passegger;A. Pavlov;S. Pedraz;D. Pérez;M. Perger;R. Rebolo;S. Reffert;E. Rodríguez;C. López;A. Rosich;S. Sabotta;S. Sadegi;M. Salz;A. Sánchez;J. Sanz;P. Sarkis;S. Schäfer;J. Schiller;J. Schmitt;P. Schöfer;A. Schweitzer;D. Shulyak;E. Solano;O. Stahl;M. T. Pinto;T. Trifonov;M. Z. Osorio;F. Yan;M. Zechmeister;F. J. Abellán;M. Abril;F. J. Alonso;F. J. Alonso;M. A. Eiff;G. Anglada;G. Anglada;H. Anwand;B. Arroyo;Z. Berdiñas;G. Bergondy;M. Blümcke;C. D. Burgo;J. Cano;J. Carro;M. Cárdenas;E. Casal;A. Claret;E. Díez;M. Doellinger;R. Dorda;C. Feiz;Matilde Fernández;I. Ferro;G. Gaisné;I. Gallardo;M. C. Gálvez;A. Garcia;M. García;R. Garrido;L. Gesa;V. Galera;E. González;E. González;L. González;S. Grohnert;U. Grözinger;J. Guàrdia;A. Guijarro;R. Hedrosa;D. Hermann;I. Hermelo;R. Arabí;F. Hernando;D. Hidalgo;D. Hidalgo;G. Holgado;G. Holgado;A. Huber;K. Huber;P. Huke;M. Kehr;M. Kim;R. Klein;J. Klüter;A. Klutsch;A. Klutsch;F. Labarga;N. Labiche;A. Lamert;W. Laun;F. Lázaro;U. Lemke;R. Lenzen;M. Llamas;J. Lizon;N. Lodieu;M. J. González;M. López;J. Salas;J. Lopez;H. M. Madinabeitia;U. Mall;L. Mancini;J. Molina;H. Martínez;H. Martínez;D. Fernández;C. Marvin;E. Mirabet;M. Moreno;A. Moya;R. Mundt;V. Naranjo;J. Panduro;J. Pascual;A. Pérez;M. Perryman;M. Pluto;A. Ramón;P. Redondo;S. Reinhart;P. Rhode;H. Rix;F. Rodler;R. Rohloff;E. Sánchez;M. A. S. Carrasco;L. Sarmiento;C. Schmidt;C. Storz;J. Strachan;J. Stürmer;J. Suárez;H. Tabernero;L. Tal;S. Tulloch;R. Ulbrich;G. Veredas;J. Linares;M. Vidal;F. Vilardell;K. Wagner;J. Winkler;V. Wolthoff;W. Xu;Z. Zhao
CARMENES 的设计和构造已在之前的 SPIE 会议上展示过。它是卡拉阿尔托天文台 3.5 m 望远镜的下一代径向速度仪器，该望远镜由 11 个西班牙和德国机构组成的联盟建造。 CARMENES 由两个独立的中阶梯光栅光谱仪组成，波长范围为 0.52 至 1.71μm，光谱分辨率为 R < 80,000，由望远镜卡塞格伦焦点的光纤馈电。 CARMENES 于 2015 年 11 月 9 日看到了“第一缕曙光”。在调试和初始运行阶段，我们建立了吞吐量和光谱分辨率等基本性能数据。我们发现我们的空心阴极灯适合精确的波长校准，但它们的光谱包含许多氖气或氩气线，这些线太亮，以至于灯不能与星星同时曝光。因此，我们采用了一种校准程序，该程序使用同步星光/法布里珀罗标准具曝光，并结合白天标准具和空心阴极灯之间的交叉校准。通过这种策略，可以在可见光中实现 1-2 m/s 的精度，在近红外中实现 5-10 m/s 的精度；预计正在进行的温度控制、校准程序和数据缩减方面的工作将进一步改进。比较不同波段中实现的 RV 精度，我们发现 0.7 至 0.8μm 之间的“最佳点”，其中深 TiO2 波段提供了中 M 矮星丰富的 RV 信息。这与我们的预调查模型形成鲜明对比，我们的预调查模型预测在 1μm 左右的近红外区域具有相对更好的性能，并部分解释了为什么我们的近红外 RV 无法达到与可见光谱仪拍摄的精度水平相同的精度水平。我们现在正在对附近的 340 个 M 矮星（平均距离只有 12%）进行大规模勘测，目标是在其宜居带内寻找类地行星。我们已经检测到了几颗先前已知或疑似行星的特征，还发现了几颗新行星。我们发现许多 M 型矮星的径向速度周期图显示出几个显着的峰值。因此，开发稳健的方法来区分行星特征和活动引起的径向速度抖动是我们的首要任务之一。由于其较大的波长覆盖范围，CARMENES 巡天正在生成一个独特的数据集，用于研究 M 星的大气、旋转和活动。光谱涵盖了重要的活性诊断线（H α、Na I D1 和 D2 以及 Ca II 红外三重态）以及 FeH 线，从中可以推断出磁场。将这些特征的时间序列相互关联，并与波长相关的径向速度相关联，为区分行星伴星和恒星径向速度抖动提供了极好的处理方法。这些数据还为 M 矮星大气的物理特性以及活动和耀斑对 M 恒星行星宜居性的影响提供了新的见解。
The design and construction of CARMENES has been presented at previous SPIE conferences. It is a next-generation radial-velocity instrument at the 3.5m telescope of the Calar Alto Observatory, which was built by a consortium of eleven Spanish and German institutions. CARMENES consists of two separate échelle spectrographs covering the wavelength range from 0.52 to 1.71μm at a spec-tral resolution of R < 80,000, fed by fibers from the Cassegrain focus of the telescope. CARMENES saw “First Light” on Nov 9, 2015. During the commissioning and initial operation phases, we established basic performance data such as throughput and spectral resolution. We found that our hollow-cathode lamps are suitable for precise wavelength calibration, but their spectra contain a number of lines of neon or argon that are so bright that the lamps cannot be used in simultaneous exposures with stars. We have therefore adopted a calibration procedure that uses simultaneous star / Fabry Pérot etalon exposures in combination with a cross-calibration between the etalons and hollow-cathode lamps during daytime. With this strategy it has been possible to achieve 1-2 m/s precision in the visible and 5-10 m/s precision in the near-IR; further improvements are expected from ongoing work on temperature control, calibration procedures and data reduction. Comparing the RV precision achieved in different wavelength bands, we find a “sweet spot” between 0.7 and 0.8μm, where deep TiO bands provide rich RV information in mid-M dwarfs. This is in contrast to our pre-survey models, which predicted comparatively better performance in the near-IR around 1μm, and explains in part why our near-IR RVs do not reach the same precision level as those taken with the visible spectrograph. We are now conducting a large survey of 340 nearby M dwarfs (with an average distance of only 12pc), with the goal of finding terrestrial planets in their habitable zones. We have detected the signatures of several previously known or suspected planets and also discovered several new planets. We find that the radial velocity periodograms of many M dwarfs show several significant peaks. The development of robust methods to distinguish planet signatures from activity-induced radial velocity jitter is therefore among our priorities. Due to its large wavelength coverage, the CARMENES survey is generating a unique data set for studies of M star atmospheres, rotation, and activity. The spectra cover important diagnostic lines for activity (H alpha, Na I D1 and D2, and the Ca II infrared triplet), as well as FeH lines, from which the magnetic field can be inferred. Correlating the time series of these features with each other, and with wavelength-dependent radial velocities, provides excellent handles for the discrimination between planetary companions and stellar radial velocity jitter. These data are also generating new insight into the physical properties of M dwarf atmospheres, and the impact of activity and flares on the habitability of M star planets.
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影响因子：
6.5
作者：
A. Reiners;I. Ribas;M. Zechmeister;J. Caballero;T. Trifonov;S. Dreizler;J. Morales;L. Tal-Or;M. Lafarga;A. Quirrenbach;P. Amado;A. Kaminski;S. Jeffers;J. Aceituno;V. Béjar;J. Guàrdia;E. Guenther;H. Hagen;D. Montes;V. Passegger;W. Seifert;A. Schweitzer;M. Cortés-Contreras;M. Cortés-Contreras;M. Abril;F. J. Alonso-Floriano;F. J. Alonso-Floriano;M. A. Eiff;R. Antona;G. Anglada-Escudé;H. Anwand-Heerwart;B. Arroyo-Torres;M. Azzaro;D. Baroch;D. Barrado;F. Bauer;S. Becerril;D. Benítez;Z. Berdiñas;G. Bergond;M. Blümcke;M. Brinkmöller;C. D. Burgo;J. Cano;M. Vázquez;M. Vázquez;E. Casal;C. Cifuentes;A. Claret;J. Colomé;S. Czesla;E. Díez-Alonso;C. Feiz;M. Fernández;I. Ferro;B. Fuhrmeister;D. Galad'i-Enr'iquez;A. Garcia-Piquer;M. Vargas;L. Gesa;V. Galera;J. Hern'andez;R. Gonz'alez-Peinado;U. Grözinger;S. Grohnert;A. Guijarro;E. D. Guindos;J. Gutiérrez-Soto;A. Hatzes;P. Hauschildt;R. Hedrosa;J. Helmling;T. Henning;I. Hermelo;R. Arabí;L. Castano;F. Hernando;E. Herrero;A. Huber;P. Huke;E. Johnson;E. Juan;M. Kim;R. Klein;J. Klüter;A. Klutsch;M. Kürster;F. Labarga;A. Lamert;M. Lamp'on;L. Lara;W. Laun;U. Lemke;R. Lenzen;R. Launhardt;M. L. D. Fresno;M. J. L'opez-Gonz'alez;M. López‐Puertas;J. F. Salas;J. Lopez-Santiago;R. Luque;H. M. Madinabeitia;U. Mall;L. Mancini;L. Mancini;H. Mandel;E. Marfil;J. Molina;D. Fernández;E. L. Martín;S. Martín-Ruiz;C. Marvin;Richard J. Mathar;E. Mirabet;M. Moreno-Raya;A. Moya;R. Mundt;E. Nagel;V. Naranjo;L. Nortmann;G. Nowak;A. Ofir;R. Oreiro;E. Pallé;J. Panduro;J. Pascual;A. Pavlov;S. Pedraz;A. Pérez-Calpena;D. P. Medialdea;M. Perger;M. Perryman;M. Pluto;O. Rabaza;O. Rabaza;A. Ramón;R. Rebolo;P. Redondo;S. Reffert;S. Reinhart;P. Rhode;H. Rix;F. Rodler;F. Rodler;E. Rodr'iguez;C. Rodríguez-López;A. R. Trinidad;R. Rohloff;A. Rosich;S. Sadegi;E. Sánchez-Blanco;M. Carrasco;A. S'anchez-L'opez;J. Sanz-Forcada;P. Sarkis;L. Sarmiento;S. Schafer;J. H. M. M. Schmitt-J.-H.-M.-M.-Schmitt-2244209165;J. Schiller;P. Schöfer;E. Solano;O. Stahl;J. Strachan;J. Stürmer;J. Suárez;J. Suárez;H. Tabernero;H. Tabernero;M. Tala;S. Tulloch;R. Ulbrich;G. Veredas;J. Linares;F. Vilardell;K. Wagner;J. Winkler;V. Wolthoff;W. Xu;F. Yan;M. Z. Osorio
通讯作者：
A. Reiners;I. Ribas;M. Zechmeister;J. Caballero;T. Trifonov;S. Dreizler;J. Morales;L. Tal-Or;M. Lafarga;A. Quirrenbach;P. Amado;A. Kaminski;S. Jeffers;J. Aceituno;V. Béjar;J. Guàrdia;E. Guenther;H. Hagen;D. Montes;V. Passegger;W. Seifert;A. Schweitzer;M. Cortés-Contreras;M. Cortés-Contreras;M. Abril;F. J. Alonso-Floriano;F. J. Alonso-Floriano;M. A. Eiff;R. Antona;G. Anglada-Escudé;H. Anwand-Heerwart;B. Arroyo-Torres;M. Azzaro;D. Baroch;D. Barrado;F. Bauer;S. Becerril;D. Benítez;Z. Berdiñas;G. Bergond;M. Blümcke;M. Brinkmöller;C. D. Burgo;J. Cano;M. Vázquez;M. Vázquez;E. Casal;C. Cifuentes;A. Claret;J. Colomé;S. Czesla;E. Díez-Alonso;C. Feiz;M. Fernández;I. Ferro;B. Fuhrmeister;D. Galad'i-Enr'iquez;A. Garcia-Piquer;M. Vargas;L. Gesa;V. Galera;J. Hern'andez;R. Gonz'alez-Peinado;U. Grözinger;S. Grohnert;A. Guijarro;E. D. Guindos;J. Gutiérrez-Soto;A. Hatzes;P. Hauschildt;R. Hedrosa;J. Helmling;T. Henning;I. Hermelo;R. Arabí;L. Castano;F. Hernando;E. Herrero;A. Huber;P. Huke;E. Johnson;E. Juan;M. Kim;R. Klein;J. Klüter;A. Klutsch;M. Kürster;F. Labarga;A. Lamert;M. Lamp'on;L. Lara;W. Laun;U. Lemke;R. Lenzen;R. Launhardt;M. L. D. Fresno;M. J. L'opez-Gonz'alez;M. López‐Puertas;J. F. Salas;J. Lopez-Santiago;R. Luque;H. M. Madinabeitia;U. Mall;L. Mancini;L. Mancini;H. Mandel;E. Marfil;J. Molina;D. Fernández;E. L. Martín;S. Martín-Ruiz;C. Marvin;Richard J. Mathar;E. Mirabet;M. Moreno-Raya;A. Moya;R. Mundt;E. Nagel;V. Naranjo;L. Nortmann;G. Nowak;A. Ofir;R. Oreiro;E. Pallé;J. Panduro;J. Pascual;A. Pavlov;S. Pedraz;A. Pérez-Calpena;D. P. Medialdea;M. Perger;M. Perryman;M. Pluto;O. Rabaza;O. Rabaza;A. Ramón;R. Rebolo;P. Redondo;S. Reffert;S. Reinhart;P. Rhode;H. Rix;F. Rodler;F. Rodler;E. Rodr'iguez;C. Rodríguez-López;A. R. Trinidad;R. Rohloff;A. Rosich;S. Sadegi;E. Sánchez-Blanco;M. Carrasco;A. S'anchez-L'opez;J. Sanz-Forcada;P. Sarkis;L. Sarmiento;S. Schafer;J. H. M. M. Schmitt-J.-H.-M.-M.-Schmitt-2244209165;J. Schiller;P. Schöfer;E. Solano;O. Stahl;J. Strachan;J. Stürmer;J. Suárez;J. Suárez;H. Tabernero;H. Tabernero;M. Tala;S. Tulloch;R. Ulbrich;G. Veredas;J. Linares;F. Vilardell;K. Wagner;J. Winkler;V. Wolthoff;W. Xu;F. Yan;M. Z. Osorio
DOI：
10.1051/0004-6361/201525803
发表时间：
2015-02
期刊：
arXiv: Solar and Stellar Astrophysics
影响因子：
--
作者：
F. J. Alonso-Floriano;J. Morales;J. Morales;J. Caballero;D. Montes;A. Klutsch;A. Klutsch;R. Mundt;M. Cortés-Contreras;I. Ribas;A. Reiners;P. Amado;A. Quirrenbach;S. Jeffers
通讯作者：
F. J. Alonso-Floriano;J. Morales;J. Morales;J. Caballero;D. Montes;A. Klutsch;A. Klutsch;R. Mundt;M. Cortés-Contreras;I. Ribas;A. Reiners;P. Amado;A. Quirrenbach;S. Jeffers
CARMENES 仪器概述
DOI：
10.1117/12.2056453
发表时间：
2014
期刊：
影响因子：
--
作者：
Quirrenbach
通讯作者：
Quirrenbach
在 CARMENES 调查中表征 U-Ne 空心阴极灯的近红外波长
DOI：
10.1117/12.2056501
发表时间：
2014
期刊：
影响因子：
--
作者：
Ramsay;Suzanne K;McLean;Takami;Hideki
通讯作者：
Hideki
CARMENES I：仪器和调查概述
DOI：
10.1117/12.925164
发表时间：
2012
期刊：
影响因子：
--
作者：
Quirrenbach;Andreas;Zechmeister;Mathias
通讯作者：
Mathias