TY - JOUR
T1 - A Deep Search for Planets in the Inner 15 au around Vega
AU - Meshkat, Tiffany
AU - Nilsson, Ricky
AU - Aguilar, Jonathan
AU - Vasisht, Gautam
AU - Oppenheimer, Rebecca
AU - Su, Kate Y.L.
AU - Cady, Eric
AU - Lockhart, Thomas
AU - Matthews, Christopher
AU - Dekany, Richard
AU - Leisenring, Jarron
AU - Ygouf, Marie
AU - Mawet, Dimitri
AU - Pueyo, Laurent
AU - Beichman, Charles
N1 - Funding Information:
We thank the anonymous referee for their helpful suggestions that improved this paper. We thank the Palomar mountain crew, especially Bruce Baker, Mike Doyle, Carolyn Heffner, John Henning, Greg van Idsinga, Steve Kunsman, Dan McKenna, Jean Mueller, Kajsa Peffer, Paul Nied, Joel Pearman, Kevin Rykoski, Carolyn Heffner, Jamey Eriksen, and Pam Thompson. We thank AAron Veicht for his contributions to the data acquisition during the observations. K.Y.L.S. acknowledges the partial support from the NASA grant NNX15AI86G. G.V. acknowledges the JPL Research & Technology Program and the NASA XRP grant 399131.02.07.02.66.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/11
Y1 - 2018/11
N2 - We present the results of a deep high-contrast imaging search for planets around Vega. Vega is an ideal target for high-contrast imaging because it is bright, nearby, and young with a face-on two-belt debris disk that may be shaped by unseen planets. We obtained J- and H-band data on Vega with the coronagraphic integral-field spectrograph Project 1640 (P1640) at Palomar Observatory. Two nights of data were obtained in 2016, in poor seeing conditions, and two additional nights in more favorable conditions in 2017. In total, we obtained 5.5 hours of integration time on Vega in moderate to good seeing conditions (<1.″5). We did not detect any low-mass companions in this system. Our data present the most sensitive contrast limits around Vega at very small separations (2-15 au) thus far, allowing us to place new constraints on the companions that may be sculpting the Vega system. In addition to new constraints, as the deepest data obtained with P1640, these observations form the final legacy of the now decommissioned instrument.
AB - We present the results of a deep high-contrast imaging search for planets around Vega. Vega is an ideal target for high-contrast imaging because it is bright, nearby, and young with a face-on two-belt debris disk that may be shaped by unseen planets. We obtained J- and H-band data on Vega with the coronagraphic integral-field spectrograph Project 1640 (P1640) at Palomar Observatory. Two nights of data were obtained in 2016, in poor seeing conditions, and two additional nights in more favorable conditions in 2017. In total, we obtained 5.5 hours of integration time on Vega in moderate to good seeing conditions (<1.″5). We did not detect any low-mass companions in this system. Our data present the most sensitive contrast limits around Vega at very small separations (2-15 au) thus far, allowing us to place new constraints on the companions that may be sculpting the Vega system. In addition to new constraints, as the deepest data obtained with P1640, these observations form the final legacy of the now decommissioned instrument.
KW - circumstellar matter
KW - planets and satellites: detection
KW - stars: individual (Vega)
KW - techniques: high angular resolution
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U2 - 10.3847/1538-3881/aae14f
DO - 10.3847/1538-3881/aae14f
M3 - Article
AN - SCOPUS:85056736462
SN - 0004-6256
VL - 156
JO - Astronomical Journal
JF - Astronomical Journal
IS - 5
M1 - 214
ER -