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A Long-Period Eccentric Substellar Companion to the Evolved Intermediate-Mass Star HD 14067

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A Long-Period Eccentric Substellar Companion to the Evolved Intermediate-Mass Star HD 14067 118-1 Publ. Astron. Soc. Japan (2014) 66 (6), 118 (1–9) doi: 10.1093/pasj/psu113 Advance Access Publication Date: 2014 December 9 A long-period eccentric substellar companion to the evolved intermediate-mass star HD 14067 Liang WANG,1 Bun’ei SATO,2 Masashi OMIYA,2 Hiroki HARAKAWA,2 Yujuan LIU,1 Nan SONG,1,3 Wei HE,1,3 Xiaoshu WU,1,3 Hideyuki IZUMIURA,4,5 Eiji KAMBE,4 Yo i ch i T AKEDA,5,6 Michitoshi YOSHIDA,7 Yo i ch i I TOH,8 ∗ Downloaded from Hiroyasu ANDO,6 Eiichiro KOKUBO,6 Shigeru IDA,2 and Gang ZHAO1, 1Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20, Datun Road, Chaoyang District, Beijing 100012, China 2Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8550, Japan http://pasj.oxfordjournals.org/ 3University of Chinese Academy of Sciences, 19A Yuquan Road, Shijingshan District, 100049 Beijing, China 4Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Kamogata-cho, Asakuchi, Okayama 719-0232, Japan 5The Graduate University for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193, Japan 6National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 7Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan at National Astronomical Observatory on January 28, 2015 8Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo, Hyogo 679-5313, Japan *E-mail: [email protected] Received 2014 July 22; Accepted 2014 September 4 Abstract We report on the detection of a substellar companion orbiting an evolved intermediate- mass (M = 2.4 M) star HD 14067 (G9 III) using a precise Doppler technique. Either a periodic Keplerian variation with a decreasing linear velocity trend (P = 1455 d, −1 −1 −1 K1 = 92.2 m s , e = 0.533, andγ ˙ =−22.4ms yr ) or a single Keplerian orbit without −1 linear trend (P = 2850 d, K1 = 100.1 m s ,ande = 0.697) can be well fitted to the radial velocities of this star. The minimum mass (m2 sin i = 7.8 MJ for the model with a linear trend, or m2 sin i = 9.0 MJ for the model without a linear trend) suggests a long-period giant planet orbiting an evolved intermediate-mass star. The eccentricity of the orbit is among the highest ones ever detected for planets moving around evolved stars. Key words: planetary systems — stars: individual (HD 14067) — techniques: radial velocities 1 Introduction past decade. Over 90 substellar companions with min- Since the first giant planet orbiting an evolved star was imum masses ranging from 0.6 to 40 MJ around giants and discovered by Frink et al. (2002), progress has been made subgiants have been detected by precise radial velocity on the detection and theoretical understanding of planets techniques (e.g., Sato et al. 2003; Setiawan et al. moving around stars more massive than our Sun in the 2003; Hatzes et al. 2005; Johnson et al. 2007, 2011; C The Author 2014. Published by Oxford University Press on behalf of the Astronomical Society of Japan. All rights reserved. For Permissions, please email: [email protected] Publications of the Astronomical Society of Japan, (2014), Vol. 66, No. 6 118-2 Sato et al. 2008b;Dollinger¨ et al. 2009; Liu et al. 2009; Japanese, Korean, and Chinese researchers using three tele- Wittenmyer et al. 2011; Omiya et al. 2012; Gettel et al. scopes in the 2 m class in 2005 (East-Asian Planet Search 2012; Lee et al. 2013; Jones et al. 2014), including those in Network: Izumiura 2005), and started the Subaru planet open clusters (e.g., Sato et al. 2007; Lovis & Mayor 2007; search program in 2006. By taking advantage of the large Brucalassi et al. 2014) and multiple-planet systems (e.g., aperture (8.2 m) of Subaru Telescope, the planet-hosting Niedzielski et al. 2009; Sato et al. 2013b) and those with candidates among a sample of ∼ 300 giants were quickly masses 13 MJ which thus lie in the brown dwarf regime identified, and the visual magnitudes of 6.5 ≤ V ≤ 7.0 (e.g., Omiya et al. 2009; Sato et al. 2010;Wangetal.2012). enabled them to be subsequently followed up by telescopes Although the number of such companions moving in the 2 m class telescopes. For details of the Subaru planet around GK giants is still insufficient to make a statistical search program, readers are referred to the description in study of their physical properties, they are of intense interest Sato et al. (2010). because their host stars are the slowly rotating counterparts We obtained a total of three spectra for HD 14067 in of intermediate-mass (1.5 < M/M < 5) B–A dwarfs that 2007 September, 2008 January, and 2008 August using the Downloaded from have evolved off the main sequence, giving us a chance High Dispersion Spectrograph (HDS: Noguchi et al. 2002) to study planets orbiting stars with masses larger than equipped with the Subaru Telescope. An iodine (I2) absorp- those of FGK dwarfs. Recent studies have revealed some tion cell was used for providing a fiducial wavelength refer- distinct differences from the FGK main sequence stars. ence for precise radial velocity measurements (Kambe et al. For instance, nearly all detected planets moving around 2002; Sato et al. 2002). We adopted the setups of StdI2b http://pasj.oxfordjournals.org/ M > 1.5 M stars have semimajor axes 0.6 au, with only in the first two runs and StdI2a in the third one, which a few exceptions including HD 102956 b (Johnson et al. covered wavelength regions of 3500–6200 A˚ and 4900– 2010), HIP 63242 (Jones et al. 2013), WASP-33 b (Collier 7600 A,˚ respectively. The slit width was set to 0.6, giving Cameron et al. 2010), and Kepler-13 Ab (Szaboetal.´ 2011). a resolving power (λ/λ) of 60000. The typical signal-to- Such paucity can be attributed to engulfment by the host noise ratio (S/N) was 140–200 pixel−1 with an exposure stars as they evolved off the main sequence (Sato et al. time of 30–50 s. 2008a; Nordhaus et al. 2010), or the primordial deficiency After the observations at the Subaru Telescope, we at National Astronomical Observatory on January 28, 2015 of short-period planets during their formation (e.g., Currie started follow-up observations using the 1.88 m telescope 2009; Kretke et al. 2009). On the other hand, most planets with the High Dispersion Echelle Spectrograph (HIDES: ever detected around intermediate-mass stars have eccen- Izumiura 1999) at OAO. The wavelength region was set to tricities below 0.4. It is natural because most of their hosts simultaneously cover 3750–7500 A˚ using the RED cross- are in the post-RGB (core helium burning) phase, and the disperser with a mosaic of three CCDs. We set the slit width planetary orbits could have been tidally circularized due to to 200 μm(0.76), giving a resolving power (λ/λ) of 67000 the increasing radii of the host star as it ascends the red with 3.3 pixel sampling, and used an iodine cell for pre- giant branch. However, some planets with a high eccen- cise wavelength calibration. We collected a total of 27 data tricity (e > 0.6) have been discovered (e.g., Sato et al. 2013a; points of HD 14067 with HIDES during the period from Moutou et al. 2011; Niedzielski et al. 2009), implying the 2008 October to 2014 January. existence of planet–planet scattering scenarios (e.g., Ford & In 2012 November we started follow-up observations of Rasio 2008) or perturbators (e.g., Takeda & Rasio 2005). HD 14067 with the High Resolution Spectrograph (HRS) In this paper, we report on the detection of a new attached at the Cassegrain focus of the 2.16 m telescope substellar companion around an intermediate-mass giant at Xinglong Observatory, China. The fiber-fed spectro- HD 14067 from our planet search program using the graph is the successor of the Coude´ Echelle Spectrograph Subaru 8.2 m telescope, the OAO 1.88 m telescope, and the (CES: Zhao & Li 2001), giving higher wavelength resolu- Xinglong 2.16 m telescope. Observations are described in tion and optical throughput. The single 4 K × 4 K CCD section 2 and stellar properties are summarized in section 3. covers a wavelength region of 3700–9200 A.˚ The slit width Analyses of radial velocities and orbital solutions are given was set to 190 μm, corresponding to a resolving power in section 4. In section 5 we give the conclusion. (λ/λ) of 45000 with 3.2 pixel sampling. An iodine cell was installed before the fiber entrance to obtain a precise wavelength reference. 2 Observations and radial velocity analysis The reduction of the echelle spectra was performed by We have been conducting a precise radial velocity survey for using the IRAF1 software package in the standard manner. about 300 G–K giants at Okayama Astrophysical Observa- 1 IRAF is distributed by the National Optical Astronomical Observatory, which is tory (OAO), Japan, since 2001. To extend this planet search operated by the Association of Universities for Research in Astronomy, Inc., under program, we established an international network among cooperative agreement with the National Science Foundation. 118-3 Publications of the Astronomical Society of Japan, (2014), Vol. 66, No. 6 The I2-superposed spectra are modeled based on the algo- rithm given by Sato et al. (2002, 2012). The stellar template used for radial velocity analysis was extracted by decon- volving an instrumental profile, which was determined from a spectrum of a B-type star taken through the I2 cell (Sato et al.
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