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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/27894
Title: The Transiting Multi-planet System HD 3167: A 5.7 M ⊕ Super-Earth and an 8.3 M ⊕ Mini-Neptune
Authors: Gandolfi, Davide
Barragán, Oscar
Hatzes, Artie P.
Fridlund, Malcolm
Fossati, Luca
Donati, Paolo
Johnson, Marshall C.
Nowak, Grzegorz
Prieto-Arranz, Jorge
Albrecht, Simon
Dai, Fei
Deeg, Hans
Endl, Michael
Grziwa, Sascha
Hjorth, Maria
Korth, Judith
Nespral, David
Saario, Joonas
Smith, Alexis M. S.
Antoniciello, Giuliano
Alarcon, Javier
Bedell, Megan
Blay, Pere
Brems, Stefan S.
Cabrera, Juan
Csizmadia, Szilard
CUSANO, FELICE 
Cochran, William D.
Eigmüller, Philipp
Erikson, Anders
González Hernández, Jonay I.
Guenther, Eike W.
Hirano, Teruyuki
Suárez Mascareño, Alejandro
Narita, Norio
Palle, Enric
Parviainen, Hannu
Pätzold, Martin
Persson, Carina M.
Rauer, Heike
Saviane, Ivo
Schmidtobreick, Linda
Van Eylen, Vincent
Winn, Joshua N.
Zakhozhay, Olga V.
Issue Date: 2017
Journal: THE ASTRONOMICAL JOURNAL 
Number: 154
Issue: 3
First Page: 123
Abstract: HD 3167 is a bright (V = 8.9 mag) K0 V star observed by NASA’s K2 space mission during its Campaign 8. It has recently been found to host two small transiting planets, namely, HD 3167b, an ultra-short-period (0.96 days) super-Earth, and HD 3167c, a mini-Neptune on a relatively long-period orbit (29.85 days). Here we present an intensive radial velocity (RV) follow-up of HD 3167 performed with the FIES@NOT, HARPS@ESO-3.6 m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69 ± 0.44 M <SUB>⊕</SUB>, a radius of 1.574 ± 0.054 R <SUB>⊕</SUB>, and a mean density of {8.00}<SUB>-0.98</SUB><SUP>+1.10</SUP> {{g}} {{cm}}<SUP>-3</SUP>, HD 3167b joins the small group of ultra-short-period planets known to have rocky terrestrial compositions. HD 3167c has a mass of {8.33}<SUB>-1.85</SUB><SUP>+1.79</SUP> M <SUB>⊕</SUB> and a radius of {2.740}<SUB>-0.100</SUB><SUP>+0.106</SUP> R <SUB>⊕</SUB>, yielding a mean density of {2.21}<SUB>-0.53</SUB><SUP>+0.56</SUP> {{g}} {{cm}}<SUP>-3</SUP>, indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (∼350 km) and the brightness of the host star make HD 3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the RV measurements but the currently available data set does not allow us to draw any firm conclusions on the origin of the observed variation.
URI: http://hdl.handle.net/20.500.12386/27894
URL: https://iopscience.iop.org/article/10.3847/1538-3881/aa832a
ISSN: 0004-6256
DOI: 10.3847/1538-3881/aa832a
Bibcode ADS: 2017AJ....154..123G
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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