Imaging Cool Giant Planets in Reflected Light: Science Investigations and Synergy with Habitable Planets. (arXiv:1903.09322v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Marley_M/0/1/0/all/0/1">Mark Marley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewis_N/0/1/0/all/0/1">Nikole Lewis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arney_G/0/1/0/all/0/1">Giada Arney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailey_V/0/1/0/all/0/1">Vanessa Bailey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batalha_N/0/1/0/all/0/1">Natasha Batalha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beichman_C/0/1/0/all/0/1">Charles Beichman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benneke_B/0/1/0/all/0/1">Björn Benneke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blecic_J/0/1/0/all/0/1">Jasmina Blecic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cahoy_K/0/1/0/all/0/1">Kerri Cahoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chilcote_J/0/1/0/all/0/1">Jeffrey Chilcote</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Domagal_Goldman_S/0/1/0/all/0/1">Shawn Domagal-Goldman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dressing_C/0/1/0/all/0/1">Courtney Dressing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">Michael Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fortney_J/0/1/0/all/0/1">Jonathan Fortney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freedman_R/0/1/0/all/0/1">Richard Freedman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gelino_D/0/1/0/all/0/1">Dawn Gelino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gizis_J/0/1/0/all/0/1">John Gizis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guyon_O/0/1/0/all/0/1">Olivier Guyon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greene_T/0/1/0/all/0/1">Thomas Greene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hammel_H/0/1/0/all/0/1">Heidi Hammel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasegawa_Y/0/1/0/all/0/1">Yasuhiro Hasegawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jovanovic_N/0/1/0/all/0/1">Nemanja Jovanovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Konopacky_Q/0/1/0/all/0/1">Quinn Konopacky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kopparapu_R/0/1/0/all/0/1">Ravi Kopparapu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_M/0/1/0/all/0/1">Michael Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_E/0/1/0/all/0/1">Eric Lopez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lunine_J/0/1/0/all/0/1">Jonathan Lunine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lupu_R/0/1/0/all/0/1">Roxana Lupu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macintosh_B/0/1/0/all/0/1">Bruce Macintosh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandt_K/0/1/0/all/0/1">Kathleen Mandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marois_C/0/1/0/all/0/1">Christian Marois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mawet_D/0/1/0/all/0/1">Dimitri Mawet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mayorga_L/0/1/0/all/0/1">Laura Mayorga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morley_C/0/1/0/all/0/1">Caroline Morley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_E/0/1/0/all/0/1">Eric Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roberge_A/0/1/0/all/0/1">Aki Roberge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serabyn_E/0/1/0/all/0/1">Eugene Serabyn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skemer_A/0/1/0/all/0/1">Andrew Skemer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stapelfeldt_K/0/1/0/all/0/1">Karl Stapelfeldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vischer_C/0/1/0/all/0/1">Channon Vischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Jason Wang</a>
Planned astronomical observatories of the 2020s will be capable of obtaining
reflected light photometry and spectroscopy of cool extrasolar giant planets.
Here we explain that such data are valuable both for understanding the origin
and evolution of giant planets as a whole and for preparing for the
interpretation of similar datasets from potentially habitable extrasolar
terrestrial planets in the decades to follow.
Planned astronomical observatories of the 2020s will be capable of obtaining
reflected light photometry and spectroscopy of cool extrasolar giant planets.
Here we explain that such data are valuable both for understanding the origin
and evolution of giant planets as a whole and for preparing for the
interpretation of similar datasets from potentially habitable extrasolar
terrestrial planets in the decades to follow.
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