J/AJ/154/224 Transiting planets in young clusters from K2 (Rizzuto+, 2017)
Zodiacal Exoplanets In Time (ZEIT).
V. A uniform search for transiting planets in young clusters observed by K2.
Rizzuto A.C., Mann A.W., Vanderburg A., Kraus A.L., Covey K.R.
<Astron. J., 154, 224 (2017)>
=2017AJ....154..224R 2017AJ....154..224R (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Associations, stellar ; Exoplanets ;
Stars, pre-main sequence ; Photometry, G band ;
Photometry, infrared ; Proper motions ; Parallaxes, trigonometric
Keywords: methods: data analysis - open clusters and associations: general -
planetary systems - planets and satellites: detections -
planets and satellites: dynamical evolution and stability -
stars : pre-main sequence
Abstract:
Detection of transiting exoplanets around young stars is more difficult
than for older systems owing to increased stellar variability. Nine
young open cluster planets have been found in the K2 data, but no
single analysis pipeline identified all planets. We have developed a
transit search pipeline for young stars that uses a transit-shaped
notch and quadratic continuum in a 12 or 24 hr window to fit both the
stellar variability and the presence of a transit. In addition, for
the most rapid rotators (Prot<2 days) we model the variability using
a linear combination of observed rotations of each star. To maximally
exploit our new pipeline, we update the membership for four stellar
populations observed by K2 (Upper Scorpius, Pleiades, Hyades, Praesepe)
and conduct a uniform search of the members. We identify all known
transiting exoplanets in the clusters, 17 eclipsing binaries, one
transiting planet candidate orbiting a potential Pleiades member, and
three orbiting unlikely members of the young clusters. Limited injection
recovery testing on the known planet hosts indicates that for the older
Praesepe systems we are sensitive to additional exoplanets as small as
1-2 R⊕, and for the larger Upper Scorpius planet host (K2-33)
our pipeline is sensitive to ∼4 R⊕ transiting planets. The lack of
detected multiple systems in the young clusters is consistent with the
expected frequency from the original Kepler sample, within our detection
limits. With a robust pipeline that detects all known planets in the
young clusters, occurrence rate testing at young ages is now possible.
Description:
We begin with all objects with available data in the relevant observing
campaigns in the K2 Ecliptic Plane Input Catalog of Huber et al.
(2016, J/ApJS/224/2).
The first step in our membership selection is to apply coarse cuts to
remove clear nonmembers. We initially reject any objects that sit
below the main sequence at the distance of each cluster in either the
(G-J, G) or (J-K, K) color-magnitude diagrams (CMDs) with a conservative
buffer of 1 mag. This rejects <5 members from the literature in each
cluster but removes the majority of the objects observed by K2 that
are not literature members.
In total, we identified 78850, and 841 candidates with membership
probabilities >50% in Hyades, Praesepe, and Pleiades, respectively,
with a >90% recovery rate of members listed in the literature in each
cluster. Table 2 lists the candidate members identified by our selection.
Objects:
------------------------------------------------------------------------
RA (ICRS) DE Designation(s)
------------------------------------------------------------------------
04 26 54.00 +15 52 00.0 Hyades = NAME Hyades Cluster
03 47 00 +24 07.0 Pleiades = Cl Melotte 22
08 40 24 +19 40.0 Praesepe = NGC 2632
16 12 -23.4 Upper Scorpius = NAME UpperSco Association
------------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 127 3462 Candidate members in the young clusters and
associations observed by K2
table3.dat 90 41 Transit signal detections among the young
cluster members from the notch filter pipeline
table4.dat 90 5 Transit signal detections among the young
cluster members from the LOCoR pipeline
--------------------------------------------------------------------------------
See also:
V/73 : Emission-Line Stars of the Orion Population (Herbig+ 1988)
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
I/317 : The PPMXL Catalog (Roeser+ 2010)
I/322 : UCAC4 Catalogue (Zacharias+, 2012)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
J/A+A/333/619 : Upper Scorpius OB association Lithium survey
(Preibisch+ 1998)
J/A+A/356/541 : T Tauri stars in the Sco-Cen OB association (Koehler+, 2000)
J/AJ/120/479 : Low-mass stars in the Upper Sco association (Ardila+, 2000)
J/AJ/124/404 : Upper Scorpius OB association Lithium survey. II.
(Preibisch, 2002)
J/AJ/126/2971 : UBVRI photometry of 131 Herbig Ae/Be (Vieira+, 2003)
J/AJ/130/1733 : Optical spectroscopy of ρ Oph stars (Wilking+, 2005)
J/AJ/131/3016 : Low-mass objects in Upper Scorpius (Slesnick+, 2006)
J/MNRAS/373/95 : ZYJHK survey of Upper Sco association (Lodieu+, 2006)
J/AJ/136/2483 : Comoving group associated with HD 141569 (Aarnio+, 2008)
J/ApJ/688/377 : Low-mass objects in Upper Scorpius. II. (Slesnick+, 2008)
J/ApJ/704/531 : The coevality of young binary systems (Kraus+, 2009)
J/A+A/515/A75 : Low-mass population in ρ Oph cloud
(Alves de Oliveira+, 2010)
J/ApJ/712/925 : Transition circumstellar disks in Ophiuchus (Cieza+, 2010)
J/A+A/527/A24 : Spectra of low-mass stars in Upper Sco (Lodieu+, 2011)
J/AJ/142/140 : Optical spectroscopy of ρ Oph stars. II.
(Erickson+, 2011)
J/ApJ/738/122 : ScoCen debris disks Around F- and G-type stars (Chen+, 2011)
J/MNRAS/416/3108 : Membership of Sco OB2 moving group (Rizzuto+, 2011)
J/ApJ/758/31 : IR photometry for members of Upper Sco (Luhman+, 2012)
J/ApJ/795/161 : Activity and rotation in Praesepe and the Hyades
(Douglas+, 2014)
J/MNRAS/448/2737 : New PMS K/M Stars in Upper Scorpius (Rizzuto+, 2015)
J/AJ/152/113 : Pleiades members with K2 light curves. I. Periods
(Rebull+, 2016)
J/AJ/152/114 : Pleiades members with K2 light curves. II. (Rebull+, 2016)
J/AJ/152/115 : Pleiades members with K2 light curves. III.
(Stauffer+, 2016)
J/ApJ/822/47 : K2 rotation periods for 65 Hyades members (Douglas+, 2016)
J/ApJS/224/2 : K2 EPIC stellar properties for 138600 targets (Huber+, 2016)
J/MNRAS/461/794 : Scorpius-Centaurus K-Type Stars (Pecaut+, 2016)
J/MNRAS/463/1780 : Exoplanet candidates in Praesepe (M 44) (Libralato+, 2016)
J/ApJ/839/92 : Praesepe members with K2 light curve data (Rebull+, 2017)
J/ApJ/842/83 : Praesepe members rotational periods from K2 LCs
(Douglas+, 2017)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- ID Young cluster or association identifier (1)
16- 24 I9 --- EPIC [202515599/212178022] EPIC identifier
26- 27 I2 h RAh Hour of Right Ascension (J2000)
29- 30 I2 min RAm Minute of Right Ascension (J2000)
32- 36 F5.2 s RAs Second of Right Ascension (J2000)
38 A1 --- DE- Sign of the Declination (J2000)
39- 40 I2 deg DEd Degree of Declination (J2000)
42- 43 I2 arcmin DEm Arcminute of Declination (J2000)
45- 48 F4.1 arcsec DEs Arcsecond of Declination (J2000)
50- 54 F5.2 mag Gmag [5.54/20.39]? Gaia DR1 G band magnitude (2)
56- 60 F5.2 mag Ksmag [4.61/15.42]? 2MASS Ks band magnitude (3)
62- 67 F6.2 mas/yr pmRA [-88.8/564.9]? Proper motion along RA (4)
69- 73 F5.2 mas/yr e_pmRA [0/21.4]? Uncertainty in pmRA
75- 80 F6.2 mas/yr pmDE [-80.7/183.2]? Proper motion along DE (4)
82- 86 F5.2 mas/yr e_pmDE [0/55.0]? Uncertainty in pmDE
88- 92 F5.1 mas plx [1.9/794.0]? Parallax
94- 98 F5.1 mas e_plx [0.2/146.3]? Uncertainty in plx
100 I1 --- f_plx [0/4]? Flag on plx (5)
102-106 F5.1 mas/yr pmRAc [-39.2/187.7]? Expected proper motion along RA
(6)
108-112 F5.1 mas/yr pmDEc [-55.7/-1.9]? Expected proper motion along DE (6)
114-116 I3 % Pmemb [1/100]? Membership probability
118 A1 --- l_Prot [<] Limit flag on Prot
119-125 F7.4 d Prot [0.0356/66.88]? Rotation period (7)
126-127 I2 --- Ref [0/32]? Reference for Upper Sco Lit. values (8)
--------------------------------------------------------------------------------
Note (1): "Upper Sco Lit." is Upper Scorpius confirmed members from the
literature. See the last column Ref for literature references.
Note (2): Gaia Collaboration et al. (2016, Cat. I/337).
Note (3): Skrutskie et al. (2006, Cat. VII/233).
Note (4): Proper motions are taken in order of availability from the Tycho-Gaia
Astrometric Solution (Gaia Collaboration et al. 2016, Cat. I/337), Hipparcos
(Perryman & ESA 1997, Cat. I/239; van Leeuwen 2007, Cat. I/311), UCAC4
(Zacharias et al. 2013, Cat. I/322), and PPMXL (Roeser et al. 2010,
Cat. I/317).
Note (5): Flag as follows:
0 = A true measurement from either TGAS or Hipparcos;
1 = Photometric distance based on (G,G-J) photometry;
2 = Photometric distance based on (r,r-J) photometry;
3 = Photometric distance based on (V,V-K) photometry;
4 = Photometric distance based on (K,J-K) photometry.
Note (6): If the candidate shares the model space velocity vector of the cluster
model.
Note (7): Rotation period measurements from Rebull et al. (2016, J/AJ/152/113)
for Pleiades, Douglas et al. (2016, J/ApJ/822/47) for Hyades, Douglas et al.
(2017, J/ApJ/842/83) for Praesepe candidates are listed if available in the
literature. The Upper Scorpius rotation periods will be in a future
publication.
Candidates not considered in these studies were visually inspected for
rotation periods smaller that 2 days, which would impact the choice of
detrending window. These objects are marked as "<2" in the table.
Note (8): Reference as follows:
0 = Pecaut & Mamajek (2016, J/MNRAS/461/794);
1 = Rizzuto et al. (2015, J/MNRAS/448/2737);
2 = Rizzuto et al. (2011, J/MNRAS/416/3108);
3 = Luhman & Mamajek (2012, J/ApJ/758/31);
4 = Aarnio et al. (2008, J/AJ/136/2483);
5 = Preibisch et al. (1998, J/A+A/333/619);
6 = Chen et al. (2011, J/ApJ/738/122);
7 = Martin et al. (2004AJ....127..449M 2004AJ....127..449M);
8 = Gregorio-Hetem et al. (1992AJ....103..549G 1992AJ....103..549G);
9 = Meyer et al. (1993AJ....105..619M 1993AJ....105..619M);
10 = Kunkel (2000, J/A+A/356/541);
11 = Martin (1998MNRAS.300..733M 1998MNRAS.300..733M);
12 = Bouvier & Appenzeller (1992A&AS...92..481B 1992A&AS...92..481B);
13 = Martin et al. (1998AJ....115..351M 1998AJ....115..351M);
14 = Kraus & Hillenbrand (2009, J/ApJ/704/531);
15 = Lodieu et al. (2006, J/MNRAS/373/95);
16 = Erickson et al. (2011, J/AJ/142/140);
17 = Slesnick et al. (2008, J/ApJ/688/377);
18 = Slesnick et al. (2006, J/AJ/131/3016);
19 = Wilking et al. (2005, J/AJ/130/1733);
20 = Alves de Oliveira (2010, J/A+A/515/A75);
21 = Cieza et al. (2010, J/ApJ/712/925);
22 = Luhman & Rieke (1999ApJ...525..440L 1999ApJ...525..440L);
23 = Doppmann et al. (2003AJ....126.3043D 2003AJ....126.3043D);
24 = Natta et al. (2002A&A...393..597N 2002A&A...393..597N);
25 = Elias et al. (1978ApJ...224..453E 1978ApJ...224..453E);
26 = Walter et al. (1994AJ....107..692W 1994AJ....107..692W);
27 = Ardila et al. (2000, J/AJ/120/479);
28 = Lodieu et al. (2011, J/A+A/527/A24);
29 = Lodieu et al. (2008MNRAS.383.1385L 2008MNRAS.383.1385L);
30 = Preibisch et al. (2002, J/AJ/124/404);
31 = Herbig & Bell (1988, Cat. V/73);
32 = Vieira et al. (2003, J/AJ/126/2971).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- EPIC [202963882/212009427] EPIC identifier
11- 13 A3 --- ID Young cluster or association short identifier
15- 16 I2 h RAh Hour of Right Ascension (J2000)
18- 19 I2 min RAm Minute of Right Ascension (J2000)
21- 25 F5.2 s RAs Second of Right Ascension (J2000)
27 A1 --- DE- Sign of the Declination (J2000)
28- 29 I2 deg DEd Degree of Declination (J2000)
31- 32 I2 arcmin DEm Arcminute of Declination (J2000)
34- 37 F4.1 arcsec DEs Arcsecond of Declination (J2000)
39- 46 F8.5 d Per [0.5111/29.0529] Period (1)
48- 59 F12.6 d T0 [56875.4/57142.9] Transit time (MJD) (1)
61- 65 F5.1 mmag Depth [0.1/179.3] Transit depth (1)
67- 71 F5.2 d Prot [0.38/23.86]? Rotation period
73- 88 A16 --- Com Comment (2)
90 A1 --- n_Com [*] Note on Com (3)
--------------------------------------------------------------------------------
Note (1): Periods, transit times, and depths from periodic transit-like signals
detected by our notch filter pipeline (table 3) and by the linear combination
of rotations pipeline (table 4).
Note (2): We list the discovery publication reporting known cluster planets from
K2 as follows:
ZEIT-I = Mann et al. 2016ApJ...818...46M 2016ApJ...818...46M;
ZEIT-II = Gaidos et al. 2017MNRAS.464..850G 2017MNRAS.464..850G;
ZEIT-III = Mann et al. 2016AJ....152...61M 2016AJ....152...61M;
ZEIT-IV = Mann et al. 2017AJ....153...64M 2017AJ....153...64M.
Other comments are defined as follows:
EB = The periodic signal is produced by an eclipsing binary system;
Nonmem = Transit signal that looks planetary but appear to be associated with
stars unlikely to be members;
NS = The transits associated with EPIC 211804579 were determined to be due
to a nearby object;
NP = We also note some nonplanetary periodic signals reported to be
produced by material at the corotation radius around three Upper Sco
stars reported in (Stauffer et al. 2017AJ....153..152S 2017AJ....153..152S).
Note (3): Note as follows:
* = EPIC 210363145 corresponds to K2-77, according to the NASA exoplanet
archive (https://exoplanetarchive.ipac.caltech.edu/); note added by CDS.
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History:
From electronic version of the journal
References:
Mann et al. Paper I. 2016ApJ...818...46M 2016ApJ...818...46M
Gaidos et al. Paper II. 2017MNRAS.464..850G 2017MNRAS.464..850G
Mann et al. Paper III. 2016AJ....152...61M 2016AJ....152...61M
Mann et al. Paper IV. 2017AJ....153...64M 2017AJ....153...64M
Mann et al. Paper VI. 2018AJ....155....4M 2018AJ....155....4M
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 14-Aug-2018