J/ApJ/835/83 K2 GAP data release. I. Campaign 1 (Stello+, 2017)
The K2 Galactic Archaeology Program data release.
I. Asteroseismic results from campaign 1.
Stello D., Zinn J., Elsworth Y., Garcia R.A., Kallinger T., Mathur S.,
Mosser B., Sharma S., Chaplin W.J., Davies G., Huber D., Jones C.D.,
Miglio A., Silva Aguirre V.
<Astrophys. J., 835, 83-83 (2017)>
=2017ApJ...835...83S 2017ApJ...835...83S (SIMBAD/NED BibCode)
ADC_Keywords: Photometry ; Surveys ; Stars, giant ; Stars, dwarfs
Keywords: Galaxy: general; planetary systems; stars: fundamental parameters;
stars: interiors; stars: oscillations including pulsations
Abstract:
NASA's K2 mission is observing tens of thousands of stars along the
ecliptic, providing data suitable for large-scale asteroseismic
analyses to inform galactic archaeology studies. Its first campaign
covered a field near the north Galactic cap, a region never covered
before by large asteroseismic-ensemble investigations, and was
therefore of particular interest for exploring this part of our
Galaxy. Here we report the asteroseismic analysis of all stars
selected by the K2 Galactic Archaeology Program during the mission's
"north Galactic cap" campaign 1. Our consolidated analysis uses six
independent methods to measure the global seismic properties, in
particular the large frequency separation and the frequency of maximum
power. From the full target sample of 8630 stars we find about 1200
oscillating red giants, a number comparable with estimates from
galactic synthesis modeling. Thus, as a valuable by-product we find
roughly 7500 stars to be dwarfs, which provide a sample well suited
for galactic exoplanet occurrence studies because they originate from
our simple and easily reproducible selection function.
Description:
All K2 Galactic Archaeology Program (GAP; Stello+ 2015ApJ...809L...3S 2015ApJ...809L...3S)
targets were observed with Kepler for about 80 days from 2014 May 30
to August 21.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 185 1262 *Seismic results and visual detection verification
of 1262 giants detected by at least one pipeline
table4.dat 28 7056 List of stars without seismic detection
(almost all dwarfs)
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Note on table3.dat: We use six independent analysis pipelines (called CAN, COR,
BHM, A2Z, SYD, and BAM) to analyze the light curves in order to extract the
large frequency separation, Δν, and the frequency of maximum power,
νmax. See section 3.1 for the description of each pipeline.
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See also:
J/A+A/506/465 : Solar-like oscillations in red giants (Hekker+, 2009)
J/ApJ/718/L97 : Early asteroseismic results from Kepler (Van Grootel+, 2010)
J/A+A/525/A131 : Solar-like oscillations in Kepler red giants (Hekker+, 2011)
J/MNRAS/412/1210 : Kepler asteroseismic targets (Molenda-Zakowicz+, 2011)
J/ApJ/765/L41 : Asteroseismic classification of KIC objects (Stello+, 2013)
J/A+A/572/A34 : Pulsating solar-like stars in Kepler (Garcia+, 2014)
J/ApJS/210/1 : Asteroseismic study of solar-type stars (Chaplin+, 2014)
J/ApJS/211/2 : Revised properties of Q1-16 Kepler targets (Huber+, 2014)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/ApJ/809/8 : Terrestrial planet occurrence rates for KOIs (Burke+, 2015)
J/AJ/152/6 : Param. of Kepler stars using LAMOST+seismic data (Wang+, 2016)
J/ApJS/224/2 : K2 EPIC stellar properties for 138600 targets (Huber+, 2016)
J/ApJ/827/50 : Kepler faint red giants (Mathur+, 2016)
http://keplerscience.arc.nasa.gov/ : Kepler & K2 Science Center
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1 A1 --- f_EPIC Flag on EPIC (1)
2- 10 I9 --- EPIC EPIC identifier
12 A1 --- Det Detection verification code (2)
14- 20 F7.3 uHz numax [3/263]?=0 Visual frequency
of maximum power (3)
22- 27 F6.3 uHz CAN-dnu [1/20]?=0 CAN frequency separation (3)
29- 33 F5.3 uHz e_CAN-dnu [0.007/0.3]?=0 Uncertainty in CAN-dnu
35- 41 F7.3 uHz CAN-numax [2/291]?=0 CAN frequency of maximum power (3)
43- 47 F5.3 uHz e_CAN-numax [0.1/10]?=0 Uncertainty in CAN-numax
49- 54 F6.3 uHz COR-dnu [1/18.6]?=0 COR frequency separation (3)
56- 60 F5.3 uHz e_COR-dnu [0.02/0.4]?=0 Uncertainty in COR-dnu
62- 68 F7.3 uHz COR-numax [5/238]?=0 COR frequency of maximum power (3)
70- 74 F5.3 uHz e_COR-numax [0.3/5.5]?=0 Uncertainty in COR-numax
76- 81 F6.3 uHz BHM-dnu [1/18.5]?=0 BHM frequency separation (3)
83- 87 F5.3 uHz e_BHM-dnu [0.03/2.1]?=0 Uncertainty in BHM-dnu
89- 95 F7.3 uHz BHM-numax [7/235]?=0 BHM frequency of maximum power (3)
97-101 F5.3 uHz e_BHM-numax [0.04/7.7]?=0 Uncertainty in BHM-numax
103-108 F6.3 uHz A2Z-dnu [1.3/22.3]?=0 A2Z frequency separation (3)
110-114 F5.3 uHz e_A2Z-dnu [0.003/2.7]?=0 Uncertainty in A2Z-dnu
116-122 F7.3 uHz A2Z-numax [11/300]?=0 A2Z frequency of maximum power (3)
124-129 F6.3 uHz e_A2Z-numax [0.5/33]?=0 Uncertainty in A2Z-numax
131-136 F6.3 uHz SYD-dnu [1/19.2]?=0 SYD frequency separation (3)
138-143 F6.3 uHz e_SYD-dnu [0.01/27.4]?=0 Uncertainty in SYD-dnu
145-151 F7.3 uHz SYD-numax [8/255]?=0 SYD frequency of maximum power (3)
153-158 F6.3 uHz e_SYD-numax [0.07/57]?=0 Uncertainty in SYD-numax
160-165 F6.3 uHz BAM-numax [1/19.6]?=0 BAM frequency of maximum power (3)
167-171 F5.3 uHz e_BAM-numax [0.02/0.8]?=0 Uncertainty in BAM-numax
173-179 F7.3 uHz BAM-dnu [3/262]?=0 BAM frequency separation (3)
181-185 F5.3 uHz e_BAM-dnu [0.05/7]?=0 Uncertainty in BAM-dnu
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Note (1):
- = the star does not follow the K2 GAP selection function.
Note (2): Code as follows:
Y = clear detection;
M = maybe detection;
N = No detection (based on visual inspection).
Note (3): A Δν (dnu) or νmax (numax) value of zero means
that no value was returned by the pipeline or visual inspection.
See Section 3.1 for details of each pipeline.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- EPIC [201122454/201964740] EPIC identifier
11- 15 F5.2 mag Kpmag [8.8/19] Kepler magnitude
17- 19 I3 % P1 Probability of star having log(g)<1.9
21- 22 I2 % P2 Probability of star having 1.9<log(g)<3.2
24- 25 I2 % P3 [0/47] Probability of star having 3.2<log(g)<4.2
27- 28 I2 % P4 Probability of star having 4.2<log(g)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 11-Aug-2017