WFRF:(Stassun K. G.)
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04757naa a2200997 4500 | |
| 001 | oai:DiVA.org:su-141395 | |
| 003 | SwePub | |
| 008 | 170426s2017 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1413952 URI |
| 024 | 7 | a https://doi.org/10.3847/1538-4357/834/2/1622 DOI |
| 040 | a (SwePub)su | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Garcia, E. Victor4 aut |
| 245 | 1 0 | a SCExAO AND GPI Y JH BAND PHOTOMETRY AND INTEGRAL FIELD SPECTROSCOPY OF THE YOUNG BROWN DWARF COMPANION TO HD 1160 |
| 264 | c 2017-01-10 | |
| 264 | 1 | b American Astronomical Society,c 2017 |
| 338 | a print2 rdacarrier | |
| 520 | a We present high signal-to-noise ratio, precise Y JH photometry and Y band (0.957-1.120 mu m) spectroscopy of HD 1160 B, a young substellar companion discovered from the Gemini NICI Planet Finding Campaign using the Subaru Coronagraphic Extreme Adaptive Optics instrument and the Gemini Planet Imager. HD 1160 B has typical mid-M dwarf-like infrared colors and a spectral type of M5.5(-0.5)(+1.0), where the blue edge of our Y band spectrum rules out earlier spectral types. Atmospheric modeling suggests HD 1160 B has an effective temperature of 3000-3100 K, a surface gravity of log g - 4-4.5, a radius of. 1.55 +/- 0.10 R-J, and a luminosity of log L/L circle dot - 2.76 +/- 0.05. Neither the primary's Hertzspring-Russell diagram position nor atmospheric modeling of HD 1160 B show evidence for a subsolar metallicity. Interpretation of the HD 1160 B spectroscopy depends on which stellar system components are used to estimate the age. Considering HD 1160 A, B and C jointly, we derive an age of 80-125 Myr, implying that HD 1160 B straddles the hydrogen-burning limit (70-90 M-J) If we consider HD 1160 A alone, younger ages (20-125 Myr) and a brown dwarf-like mass (35-90 M-J) are possible. Interferometric measurements of the primary, a precise Gaia parallax, and moderate-resolution spectroscopy can better constrain the system's age and how HD 1160 B fits within the context of (sub) stellar evolution. | |
| 650 | 7 | a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng |
| 653 | a instrumentation: adaptive optics | |
| 653 | a planetary systems | |
| 653 | a stars: low-mass | |
| 653 | a techniques: imaging spectroscopy | |
| 700 | 1 | a Currie, Thayne4 aut |
| 700 | 1 | a Guyon, Olivier4 aut |
| 700 | 1 | a Stassun, Keivan G.4 aut |
| 700 | 1 | a Jovanovic, Nemanja4 aut |
| 700 | 1 | a Lozi, Julien4 aut |
| 700 | 1 | a Kudo, Tomoyuki4 aut |
| 700 | 1 | a Doughty, Danielle4 aut |
| 700 | 1 | a Schlieder, Josh4 aut |
| 700 | 1 | a Kwon, J.4 aut |
| 700 | 1 | a Uyama, T.4 aut |
| 700 | 1 | a Kuzuhara, M.4 aut |
| 700 | 1 | a Carson, J. C.4 aut |
| 700 | 1 | a Nakagawa, T.4 aut |
| 700 | 1 | a Hashimoto, J.4 aut |
| 700 | 1 | a Kusakabe, N.4 aut |
| 700 | 1 | a Abe, L.4 aut |
| 700 | 1 | a Brandner, W.4 aut |
| 700 | 1 | a Brandt, T. D.4 aut |
| 700 | 1 | a Feldt, M.4 aut |
| 700 | 1 | a Goto, M.4 aut |
| 700 | 1 | a Grady, C. A.4 aut |
| 700 | 1 | a Hayano, Y.4 aut |
| 700 | 1 | a Hayashi, M.4 aut |
| 700 | 1 | a Hayashi, S. S.4 aut |
| 700 | 1 | a Henning, T.4 aut |
| 700 | 1 | a Hodapp, K. W.4 aut |
| 700 | 1 | a Ishii, M.4 aut |
| 700 | 1 | a Iye, M.4 aut |
| 700 | 1 | a Janson, Markusu Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)mjanso |
| 700 | 1 | a Kandori, R.4 aut |
| 700 | 1 | a Knapp, G. R.4 aut |
| 700 | 1 | a Matsuo, T.4 aut |
| 700 | 1 | a McElwain, M. W.4 aut |
| 700 | 1 | a Miyama, S.4 aut |
| 700 | 1 | a Morino, J. -I.4 aut |
| 700 | 1 | a Moro-Martin, A.4 aut |
| 700 | 1 | a Nishimura, T.4 aut |
| 700 | 1 | a Pyo, T. -S.4 aut |
| 700 | 1 | a Serabyn, E.4 aut |
| 700 | 1 | a Suenaga, T.4 aut |
| 700 | 1 | a Suto, H.4 aut |
| 700 | 1 | a Suzuki, R.4 aut |
| 700 | 1 | a Takahashi, Y. H.4 aut |
| 700 | 1 | a Takami, H.4 aut |
| 700 | 1 | a Takami, M.4 aut |
| 700 | 1 | a Takato, N.4 aut |
| 700 | 1 | a Terada, H.4 aut |
| 700 | 1 | a Thalmann, C.4 aut |
| 700 | 1 | a Turner, E. L.4 aut |
| 700 | 1 | a Watanabe, M.4 aut |
| 700 | 1 | a Wisniewski, J.4 aut |
| 700 | 1 | a Yamada, T.4 aut |
| 700 | 1 | a Usuda, T.4 aut |
| 700 | 1 | a Tamura, M.4 aut |
| 710 | 2 | a Stockholms universitetb Institutionen för astronomi4 org |
| 773 | 0 | t Astrophysical Journald : American Astronomical Societyg 834:2q 834:2x 0004-637Xx 1538-4357 |
| 856 | 4 | u https://repository.arizona.edu/bitstream/10150/623097/1/Garcia_2017_ApJ_834_162.pdf |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-141395 |
| 856 | 4 8 | u https://doi.org/10.3847/1538-4357/834/2/162 |
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- Abe, L.
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- Brandt, T. D.
- Feldt, M.
- Goto, M.
- Grady, C. A.
- Hayano, Y.
- Hayashi, M.
- Hayashi, S. S.
- Henning, T.
- Hodapp, K. W.
- Ishii, M.
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- Janson, Markus
- Kandori, R.
- Knapp, G. R.
- Matsuo, T.
- McElwain, M. W.
- Miyama, S.
- Morino, J. -I.
- Moro-Martin, A.
- Nishimura, T.
- Pyo, T. -S.
- Serabyn, E.
- Suenaga, T.
- Suto, H.
- Suzuki, R.
- Takahashi, Y. H.
- Takami, H.
- Takami, M.
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- Terada, H.
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- Turner, E. L.
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