J/AJ/158/13 The first 300 stars observed by the GPIES (Nielsen+, 2019)
The Gemini Planet Imager Exoplanet Survey: giant planet and brown dwarf
demographics from 10 to 100 au.
Nielsen E.L., De Rosa R.J., Macintosh B., Wang J.J., Ruffio J.-B.,
Chiang E., Marley M.S., Saumon D., Savransky D., Ammons S.M., Bailey V.P.,
Barman T., Blain C., Bulger J., Burrows A., Chilcote J., Cotten T.,
Czekala I., Doyon R., Duchene G., Esposito T.M., Fabrycky D.,
Fitzgerald M.P., Follette K.B., Fortney J.J., Gerard B.L., Goodsell S.J.,
Graham J.R., Greenbaum A.Z., Hibon P., Hinkley S., Hirsch L.A., Hom J.,
Hung L.-W., Dawson R.I., Ingraham P., Kalas P., Konopacky Q., Larkin J.E.,
Lee E.J., Lin J.W., Maire J., Marchis F., Marois C., Metchev S.,
Millar-Blanchaer M.A., Morzinski K.M., Oppenheimer R., Palmer D.,
Patience J., Perrin M., Poyneer L., Pueyo L., Rafikov R.R., Rajan A.,
Rameau J., Rantakyro F.T., Ren B., Schneider A.C., Sivaramakrishnan A.,
Song I., Soummer R., Tallis M., Thomas S., Ward-Duong K., Wolff S.
<Astron. J., 158, 13 (2019)>
=2019AJ....158...13N 2019AJ....158...13N (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, brown dwarf ; Spectral types ;
Stars, distances ; Photometry, RI ; Photometry, infrared ;
Stars, ages ; Stars, masses ; Exoplanets ; Surveys
Keywords: instrumentation: adaptive optics - planetary systems -
planets and satellites: detection
Abstract:
We present a statistical analysis of the first 300 stars observed by
the Gemini Planet Imager Exoplanet Survey. This subsample includes six
detected planets and three brown dwarfs; from these detections and our
contrast curves we infer the underlying distributions of substellar
companions with respect to their mass, semimajor axis, and host stellar
mass. We uncover a strong correlation between planet occurrence rate and
host star mass, with stars M*>1.5 M☉ more likely to host planets
with masses between 2 and 13 MJup and semimajor axes of 3-100 au at
99.92% confidence. We fit a double power-law model in planet mass (m)
and semimajor axis (a) for planet populations around high-mass stars
(M*>1.5 M☉) of the form
d2N/(dm da)∝mααβ, finding α=-2.4±0.8
and β=-2.0±0.5, and an integrated occurrence rate of 9-4+5%
between 5-13 MJup and 10-100 au. A significantly lower occurrence rate
is obtained for brown dwarfs around all stars, with 0.8-0.5+0.8% of
stars hosting a brown dwarf companion between 13-80 MJup and 10-100 au.
Brown dwarfs also appear to be distributed differently in mass and
semimajor axis compared to giant planets; whereas giant planets follow
a bottom-heavy mass distribution and favor smaller semimajor axes,
brown dwarfs exhibit just the opposite behaviors. Comparing to studies
of short-period giant planets from the radial velocity method, our results
are consistent with a peak in occurrence of giant planets between ∼1 and
10 au. We discuss how these trends, including the preference of giant
planets for high-mass host stars, point to formation of giant planets
by core/pebble accretion, and formation of brown dwarfs by gravitational
instability.
Description:
The Gemini Planet Imager (GPI) is an instrument optimized to directly
detect planets at high contrast within ∼1" radius from their parent star.
The Gemini Planet Imager Exoplanet Survey (GPIES) utilizes GPI for a
600-star survey, begun in late 2014 and set to conclude in 2019
(Macintosh et al. 2018SPIE10703E..0KM). Based at Gemini South at Cerro
Pachon, Chile, GPIES is targeting the youngest, closest stars in the sky
in a systematic survey for giant planets between 10 and 100 au. Here
we present the results from the first 300 stars observed by GPIES. As
the first half of the planned survey, 300 stars represents the natural
midcourse point to consider the occurrence rate of giant planets partway
through the survey. The 300th star was observed on UT 2016-09-21, and
in this work we consider only GPIES campaign observations on or before
this date.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 144 331 300-star sample properties and observing log
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See also:
III/135 : Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989)
III/171 : MK Classifications for F- and G-type stars (Harlan, 1969-1981)
III/31 : Michigan catalogue for the HD stars, vol. 1 (Houk+, 1975)
III/51 : Michigan Catalogue of HD stars, Vol.2 (Houk, 1978)
III/80 : Michigan Catalogue of HD stars, Vol.3 (Houk, 1982)
III/117 : MK Classifications of Close Visual Binaries (Corbally, 1984)
III/133 : Michigan Catalogue of HD stars, Vol.4 (Houk+, 1988)
III/150 : Perkins Revised MK Types for the Cooler Stars (Keenan+ 1989)
III/214 : Michigan Catalogue of HD stars, Vol.5 (Houk+, 1999)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
B/mk : Catalogue of Stellar Spectral Classifications (Skiff, 2009- )
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/107/1556 : Late B-type stars classification (Garrison+, 1994)
J/ApJS/99/135 : Rotation and Spectral Peculiarities (Abt+ 1995)
J/A+A/373/625 : uvbyβ photometry of lambda Bootis stars
(Paunzen+, 2001)
J/AJ/126/2048 : NStars project: the Northern Sample. I. (Gray+, 2003)
J/A+A/460/695 : Search for Associations Containing Young stars
(Torres+, 2006)
J/AJ/132/161 : NStars project: The southern sample. I. (Gray+, 2006)
J/MNRAS/371/252 : Southern B and Be stars (Levenhagen+, 2006)
J/ApJS/180/117 : MK classifications of spectroscopic binaries (Abt, 2009)
J/AZh/88/34 : Long-term (1984-2008) JHKLM photometry of stars
(Shenavrin+, 2011)
J/AJ/145/102 : Spectroscopy of bright M dwarfs in the northern sky
(Lepine+, 2013)
J/ApJ/762/88 : Young stellar kinematic group candidate members
(Malo+, 2013)
J/MNRAS/435/1325 : Membership of the ε Cha association
(Murphy+, 2013)
J/MNRAS/454/593 : Young moving groups in solar neighbourhood (Bell+, 2015)
J/other/PASA/32.36 : lambda Boo star membership evaluations (Murphy+, 2015)
J/other/Sci/350.64 : 51 Eri b near-infrared spectrum (Macintosh+, 2015)
J/MNRAS/461/794 : Scorpius-Centaurus K-Type Stars (Pecaut+, 2016)
J/AJ/155/226 : Gemini Planet Imager spectra of HR 8799 c/d/e
(Greenbaum+, 2018)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Source name
18- 19 I2 h RAh Hour of Right Ascension (J2000)
21- 22 I2 min RAm Minute of Right Ascension (J2000)
24- 28 F5.2 s RAs Second of Right Ascension (J2000)
30 A1 --- DE- Sign of the Declination (J2000)
31- 32 I2 deg DEd Degree of Declination (J2000)
34- 35 I2 arcmin DEm Arcminute of Declination (J2000)
37- 40 F4.1 arcsec DEs Arcsecond of Declination (J2000)
42- 56 A15 --- SpType Spectral type
58- 59 A2 --- r_SpType Reference for SpType (1)
61- 68 F8.4 pc Dist [3.2161/176.67] Stellar distance
70- 75 F6.4 pc e_Dist [0.0017/8.23] Uncertainty in Dist
77- 78 A2 --- r_Dist Reference for Dist (1)
80- 82 F3.1 mag Imag [0.8/9.3] Apparent I band magnitude
84- 86 F3.1 mag Hmag [0.9/8.1] Apparent H band magnitude
88-100 A13 --- MGroup Moving group
102-104 I3 Myr Age [4/925] Stellar age
106-107 I2 --- r_Age [2/40] Reference for Age (1)
109-112 F4.2 Msun Mass [0.29/9.69] Stellar mass
114-114 A1 --- f_Mass [d] Flag indicating Mass is for the system
116-125 A10 "date" Date UT observation date
127-130 F4.1 s Exp [2.9/59.6] Exposure time
132-133 I2 --- Nco [1/10] Number of coadds
135-138 F4.1 min Tint [6/78.5] Integration time
140-144 F5.1 deg DelPA [1.7/176]? Total amount of field rotation
ΔPA
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Note (1): Reference as follows:
1 = Houk & Swift 1999, Cat. III/214;
2 = Gaia Collaboration et al. 2018, Cat. I/345;
3 = This study (SED fitting);
4 = Torres et al. 2006, J/A+A/460/695;
5 = Bell et al. 2015, J/MNRAS/454/593;
6 = Nielsen et al. 2016AJ....152..175N 2016AJ....152..175N;
7 = Zuckerman et al. 2006ApJ...649L.115Z 2006ApJ...649L.115Z;
8 = Keenan & McNeil 1989, Cat. III/150;
9 = This study (activity);
10 = Gray et al. 2006, J/AJ/132/161;
11 = van Leeuwen 2007, Cat. I/311;
12 = Gray & Garrison 1987ApJS...65..581G 1987ApJS...65..581G;
13 = Houk & Cowley 1975, Cat. III/31;
14 = Abt & Morrell 1995, J/ApJS/99/135;
15 = No reference cited in SIMBAD;
16 = Houk & Smith-Moore 1988, Cat. III/133;
17 = Barrado y Navascues et al. 2004ApJ...614..386B 2004ApJ...614..386B;
18 = Garrison & Gray 1994, J/AJ/107/1556;
19 = Schlieder et al. 2012AJ....143..114S 2012AJ....143..114S;
20 = Harlan 1974, Cat. III/171;
21 = Opolski 1957ArA.....2...55O 1957ArA.....2...55O;
22 = Houk 1982, Cat. III/80;
23 = Shenavrin et al. 2011, J/AZh/88/34;
24 = Stephenson 1986AJ.....92..139S 1986AJ.....92..139S;
25 = Hoffleit et al. 1970TOYal..30....1H 1970TOYal..30....1H;
26 = Gray & Garrison 1989ApJS...70..623G 1989ApJS...70..623G;
27 = Houk 1978, Cat. III/51;
28 = Lepine et al. 2013, J/AJ/145/102;
29 = Davison et al. 2015AJ....149..106D 2015AJ....149..106D;
30 = Abt 2009, J/ApJS/180/117;
31 = Corbally 1984, Cat. III/117;
32 = Kirkpatrick et al. 1991ApJS...77..417K 1991ApJS...77..417K;
33 = Pecaut & Mamajek 2016, J/MNRAS/461/794;
34 = Sreedhar Rao & Abhyankar 1991JApA...12..133S 1991JApA...12..133S;
35 = Paunzen et al. 2001, J/A+A/373/625;
36 = Levenhagen & Leister 2006, J/MNRAS/371/252;
37 = Harlan & Taylor 1970, Cat. III/171;
38 = Murphy et al. 2013, J/MNRAS/435/1325;
39 = Murphy et al. 2015, J/other/PASA/32.36;
40 = Weinberger et al. 1999ApJ...525L..53W 1999ApJ...525L..53W;
41 = Gray et al. 2003, J/AJ/126/2048;
42 = Stock & Wroblewski 1972PDAUC...2...59S 1972PDAUC...2...59S;
43 = Joy & Abt 1974ApJS...28....1J 1974ApJS...28....1J;
44 = Lowrance et al. 2000ApJ...541..390L 2000ApJ...541..390L;
45 = Skiff 2014, Cat. B/mk;
46 = Cannon & Pickering 1993, Cat. III/135.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 26-Aug-2019