β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b

Maxwell A. Millar-Blanchaer; James R. Graham; Laurent Pueyo; Paul Kalas; Rebekah I. Dawson; Jason Wang; Marshall D. Perrin; Dae Sik Moon; Bruce Macintosh; S. Mark Ammons; Travis Barman; Andrew Cardwell; Christine H. Chen; Eugene Chiang; Jeffrey Chilcote; Tara Cotten; Robert J.De Rosa; Zachary H. Draper; Jennifer Dunn; Gaspard Duchêne; Thomas M. Esposito; Michael P. Fitzgerald; Katherine B. Follette; Stephen J. Goodsell; Alexandra Z. Greenbaum; Markus Hartung; Pascale Hibon; Sasha Hinkley; Patrick Ingraham; Rebecca Jensen-Clem; Quinn Konopacky; James E. Larkin; Douglas Long; Jérôme Maire; Franck Marchis; Mark S. Marley; Christian Marois; Katie M. Morzinski; Eric L. Nielsen; David W. Palmer; Rebecca Oppenheimer; Lisa Poyneer; Abhijith Rajan; Fredrik T. Rantakyrö; Jean Baptiste Ruffio; Naru Sadakuni; Leslie Saddlemyer; Adam C. Schneider; Anand Sivaramakrishnan; Remi Soummer; Sandrine Thomas; Gautam Vasisht; David Vega; J. Kent Wallace; Kimberly Ward-Duong; Sloane J. Wiktorowicz; Schuyler G. Wolff

doi:10.1088/0004-637X/811/1/18

β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b

Maxwell A. Millar-Blanchaer, James R. Graham, Laurent Pueyo, Paul Kalas, Rebekah I. Dawson, Jason Wang, Marshall D. Perrin, Dae Sik Moon, Bruce Macintosh, S. Mark Ammons, Travis Barman, Andrew Cardwell, Christine H. Chen, Eugene Chiang, Jeffrey Chilcote, Tara Cotten, Robert J.De Rosa, Zachary H. Draper, Jennifer Dunn, Gaspard DuchêneThomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen J. Goodsell, Alexandra Z. Greenbaum, Markus Hartung, Pascale Hibon, Sasha Hinkley, Patrick Ingraham, Rebecca Jensen-Clem, Quinn Konopacky, James E. Larkin, Douglas Long, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Katie M. Morzinski, Eric L. Nielsen, David W. Palmer, Rebecca Oppenheimer, Lisa Poyneer, Abhijith Rajan, Fredrik T. Rantakyrö, Jean Baptiste Ruffio, Naru Sadakuni, Leslie Saddlemyer, Adam C. Schneider, Anand Sivaramakrishnan, Remi Soummer, Sandrine Thomas, Gautam Vasisht, David Vega, J. Kent Wallace, Kimberly Ward-Duong, Sloane J. Wiktorowicz, Schuyler G. Wolff

Astronomy & Astrophysics

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Abstract

We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.

Original language	English (US)
Article number	18
Journal	Astrophysical Journal
Volume	811
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/811/1/18
State	Published - Sep 20 2015

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/0004-637X/811/1/18

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Millar-Blanchaer, M. A., Graham, J. R., Pueyo, L., Kalas, P., Dawson, R. I., Wang, J., Perrin, M. D., Moon, D. S., Macintosh, B., Ammons, S. M., Barman, T., Cardwell, A., Chen, C. H., Chiang, E., Chilcote, J., Cotten, T., Rosa, R. J. D., Draper, Z. H., Dunn, J., ... Wolff, S. G. (2015). β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b. Astrophysical Journal, 811(1), Article 18. https://doi.org/10.1088/0004-637X/811/1/18

@article{d61925afdfba46019cdb999b39b43750,

title = "β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b",

abstract = "We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.",

author = "Millar-Blanchaer, {Maxwell A.} and Graham, {James R.} and Laurent Pueyo and Paul Kalas and Dawson, {Rebekah I.} and Jason Wang and Perrin, {Marshall D.} and Moon, {Dae Sik} and Bruce Macintosh and Ammons, {S. Mark} and Travis Barman and Andrew Cardwell and Chen, {Christine H.} and Eugene Chiang and Jeffrey Chilcote and Tara Cotten and Rosa, {Robert J.De} and Draper, {Zachary H.} and Jennifer Dunn and Gaspard Duch{\^e}ne and Esposito, {Thomas M.} and Fitzgerald, {Michael P.} and Follette, {Katherine B.} and Goodsell, {Stephen J.} and Greenbaum, {Alexandra Z.} and Markus Hartung and Pascale Hibon and Sasha Hinkley and Patrick Ingraham and Rebecca Jensen-Clem and Quinn Konopacky and Larkin, {James E.} and Douglas Long and J{\'e}r{\^o}me Maire and Franck Marchis and Marley, {Mark S.} and Christian Marois and Morzinski, {Katie M.} and Nielsen, {Eric L.} and Palmer, {David W.} and Rebecca Oppenheimer and Lisa Poyneer and Abhijith Rajan and Rantakyr{\"o}, {Fredrik T.} and Ruffio, {Jean Baptiste} and Naru Sadakuni and Leslie Saddlemyer and Schneider, {Adam C.} and Anand Sivaramakrishnan and Remi Soummer and Sandrine Thomas and Gautam Vasisht and David Vega and Wallace, {J. Kent} and Kimberly Ward-Duong and Wiktorowicz, {Sloane J.} and Wolff, {Schuyler G.}",

year = "2015",

month = sep,

day = "20",

doi = "10.1088/0004-637X/811/1/18",

language = "English (US)",

volume = "811",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

Millar-Blanchaer, MA, Graham, JR, Pueyo, L, Kalas, P, Dawson, RI, Wang, J, Perrin, MD, Moon, DS, Macintosh, B, Ammons, SM, Barman, T, Cardwell, A, Chen, CH, Chiang, E, Chilcote, J, Cotten, T, Rosa, RJD, Draper, ZH, Dunn, J, Duchêne, G, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, SJ, Greenbaum, AZ, Hartung, M, Hibon, P, Hinkley, S, Ingraham, P, Jensen-Clem, R, Konopacky, Q, Larkin, JE, Long, D, Maire, J, Marchis, F, Marley, MS, Marois, C, Morzinski, KM, Nielsen, EL, Palmer, DW, Oppenheimer, R, Poyneer, L, Rajan, A, Rantakyrö, FT, Ruffio, JB, Sadakuni, N, Saddlemyer, L, Schneider, AC, Sivaramakrishnan, A, Soummer, R, Thomas, S, Vasisht, G, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ & Wolff, SG 2015, 'β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b', Astrophysical Journal, vol. 811, no. 1, 18. https://doi.org/10.1088/0004-637X/811/1/18

TY - JOUR

T1 - β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b

AU - Millar-Blanchaer, Maxwell A.

AU - Graham, James R.

AU - Pueyo, Laurent

AU - Kalas, Paul

AU - Dawson, Rebekah I.

AU - Wang, Jason

AU - Perrin, Marshall D.

AU - Moon, Dae Sik

AU - Macintosh, Bruce

AU - Ammons, S. Mark

AU - Barman, Travis

AU - Cardwell, Andrew

AU - Chen, Christine H.

AU - Chiang, Eugene

AU - Chilcote, Jeffrey

AU - Cotten, Tara

AU - Rosa, Robert J.De

AU - Draper, Zachary H.

AU - Dunn, Jennifer

AU - Duchêne, Gaspard

AU - Esposito, Thomas M.

AU - Fitzgerald, Michael P.

AU - Follette, Katherine B.

AU - Goodsell, Stephen J.

AU - Greenbaum, Alexandra Z.

AU - Hartung, Markus

AU - Hibon, Pascale

AU - Hinkley, Sasha

AU - Ingraham, Patrick

AU - Jensen-Clem, Rebecca

AU - Konopacky, Quinn

AU - Larkin, James E.

AU - Long, Douglas

AU - Maire, Jérôme

AU - Marchis, Franck

AU - Marley, Mark S.

AU - Marois, Christian

AU - Morzinski, Katie M.

AU - Nielsen, Eric L.

AU - Palmer, David W.

AU - Oppenheimer, Rebecca

AU - Poyneer, Lisa

AU - Rajan, Abhijith

AU - Rantakyrö, Fredrik T.

AU - Ruffio, Jean Baptiste

AU - Sadakuni, Naru

AU - Saddlemyer, Leslie

AU - Schneider, Adam C.

AU - Sivaramakrishnan, Anand

AU - Soummer, Remi

AU - Thomas, Sandrine

AU - Vasisht, Gautam

AU - Vega, David

AU - Wallace, J. Kent

AU - Ward-Duong, Kimberly

AU - Wiktorowicz, Sloane J.

AU - Wolff, Schuyler G.

PY - 2015/9/20

Y1 - 2015/9/20

N2 - We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.

AB - We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.

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U2 - 10.1088/0004-637X/811/1/18

DO - 10.1088/0004-637X/811/1/18

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VL - 811

JO - Astrophysical Journal

JF - Astrophysical Journal

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M1 - 18

ER -

β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b

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