The Kepler Asteroseismic Science Operations Center provides asteroseismological data from the NASA Kepler mission to astronomers who are members of the Kepler Asteroseismic Science Consortium (KASC).

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In order to have access to the Kepler Asteroseismic data you have to be a member of KASC. Please see the "New KASC member" page on how to become a member.


3rd Jan 2017: K2 campaign 10 data available

Data from campaign 10 of K2 has been made available on KASOC. The data release notes have not yet been made available, but we will provide it as soon as it is available.

Please note that there are a few unique features in the C10 data:

  • The first six days of data, dubbed C10.1, were collected with a pointing error of 3.3 pixels from the nominal field-of-view, so they were only processed through CAL to make "Type 1" target pixel files. Among other things, this means that there are no light-curves produced by the K2 Science Office.
  • The remainder of the campaign, dubbed C10.2, was processed through the entire photometry pipeline, creating "Type 2" target pixel files and long-cadence light curves.
  • Module 4 was lost part way through C10.2, which powered off the photometer and produced a 14-day data gap.

14th Dec 2016: Scheduled downtime

Tomorrow (15/12-2016) we will be doing some scheduled maintenance of our systems, so the KASOC website will be unavailable for a few hours. We apologize for the inconvenience.

13th Dec 2016: Reprocessed data for K2 C1

Reprocessed data for K2 Campaign 1 (Data Release 14) is now available for download.

This release corrects the short cadence pixel calibration bug previously described in the Global Erratum for Kepler Q0-Q17 & K2 C0-C5 Short-Cadence Data (KSCI-19080). The new release also includes lightcurves for all long cadence data, plus improvements to the target pixel files.

Please have a careful read of the Data Release Notes.

Kepler & K2 News

16th Apr 2017: Release of dithered data obtained during Kepler commissioning

During Kepler’s commissioning phase in April 2009, the spacecraft observed 33,424 stars in a dither pattern for the purpose of measuring the Pixel Response Function (PRF). The pattern consisted of 122 pointings, each with a duration of 14.7 minutes, observed across a 2.5-day period on April 27-29, 2009.

The PRF inferred from these data was previously released in the form of FITS files which provide PRF images for the four corners and the center of each CCD channel. These files have been available from the Kepler data archive's Focal Plane Characteristics page for several years, and their construction was detailed in a paper by Bryson et al. 2011.

The dithered data from which the PRF was inferred was hitherto unavailable. As part of an ongoing effort to unearth all useful data before the end of the mission, these cadences have been processed into Target Pixel Files and are now available from the data archive at MAST for the first time. They may be of use to anyone wishing to investigate Kepler's intra- and inter-pixel variations. Details of this release are described in document KSCI-19100.

The animation below shows example data obtained as part of the dither sequence. The graph elucidates the dither pattern (Figure 3 from Bryson et al. 2011).

Read more

27th Mar 2017: Request for input on the Campaign 17 and 18 field placement

The fields for K2 Campaigns 17 and beyond have not yet been set. Although these future Campaigns are at risk of not being executed due to Kepler running low on fuel, there is a significant chance that the spacecraft will continue to function well into 2018 and the project must be ready to observe fields accordingly.

We strive to optimize these future fields based on potential science. We are now soliciting feedback from the community on the placement of fields 17 and 18. Example options which satisfy K2's pointing constraints are shown below. When submitting your input, please keep in mind that we can only shift the field along the ecliptic between these options, not up or down.

We ask that all requests for field placements be received by April 11 and be submitted via this Google Form. Advocacy that was submitted in recent months via e-mail will be taken into account as well. We anticipate announcing the final field positions in early May.

Questions may be addressed to keplergo@mail.arc.nasa.gov.

Campaign 17: Example forward-facing options

Campaign 17 is designated to have a forward-facing field to enable simultaneous observations from the Earth. Possible field options are outlined in the table below.

Note that all options have a start date of 3 March 2018, i.e. 5 days after the end of Campaign 16. The first option is very short in duration due to its partial overlap in observing geometry with C16.

Campaign 17: Example options
Option Possible dates Max. duration Overlap region 1 Mar 3 - Apr 18, 2018 46 days 14 modules of C10 2 Mar 3 - May 8, 2018 66 days 14 modules of C6 3 Mar 3 - May 23, 2018 81 days 1 module of C6

Campaign 18: Example forward-facing options

The field for Campaign 18 largely depends on the location of the Campaign 17 field as well as whether or not Campaign 18 will be posited as a forward-facing or backward-facing field. If we allow Campaign 18 to begin 5 days after the end of each of the three options for Campaign 17 noted above, then we obtain the following options listed below in the case of a forward-facing field:

Campaign 18: Example options (forward-facing)
Option Possible dates Max. duration Overlap region 1 Apr 23 - Jul 18, 2018 86 days 17 modules of C9* 2 May 13 - Aug 09, 2018 88 days 9 modules of C7 3 May 28 - Aug 25, 2018 88 days none * C9 was the microlensing experiment where pixels were primarily collected around the Galactic bulge. Therefore, the distribution of targets across modules was not uniform in that campaign.

Campaign 18: Example backward-facing options

And these are the C18 options for the backward-facing geometry, in which case Earth is kept out of the field but simultaneous observations from the ground would be challenging:

Campaign 18: Example options (backward-facing)
Option Possible dates Max. duration Overlap region 1 Apr 23 - Jul 18, 2018 86 days 1/2 module of C5 2 May 13 - Aug 09, 2018 88 days 14 modules of C5 and C16 3 May 28 - Aug 25, 2018 88 days 2 modules of C14


The above field options have been configured in the GitHub version of K2fov using mock field numbers:

  • 171, 172, 173 (C17);
  • 181, 182, 183 (C18 forward-facing);
  • 184, 185, 186 (C18 backward-facing).

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27th Mar 2017: Kepler DR 25 KOI Catalog now available

The latest version of the Kepler Objects of Interest (KOI) Catalog, version DR25, is now available in the NASA Exoplanet Archive.

The catalog details all the transit-like features across the full data set of the original Kepler mission, i.e. Quarters 1 through 17, as found by the Kepler pipeline and vetted by the RoboVetter. Details on the nature and contents of the catalog can be found in the DR25 KOI Companion Document.

The catalog will be the first of its kind to be accompanied by a full suite of detection reliability and completeness measurements, and will hence be the recommended catalog for estimating planet occurence rates. A first set of these accompanying products have been released alongside the catalog, and additional products will be released as they become available over the next months.

Further details on the DR25 data products, and their use for occurence rates measurements, will be described in a forthcoming paper and accompanying talks to be presented at the Kepler & K2 Science Conference IV. (Note: abstract and foreign registration deadline: March 31!)

Read more

Recently published scientific publications

  • B. Mosser: Period spacings in red giants III. Coupling factors of mixed modes
    Updated: Sat 22nd April 2017 18:52.
  • B. Mosser: When dipole modes in red giants are simultaneously mixed and depressed
    Updated: Sat 22nd April 2017 18:52.
  • Víctor Silva Aguirre: Standing on the shoulders of dwarfs: the Kepler asteroseismic LEGACY sample II — radii, masses, and ages
    Updated: Fri 7th April 2017 15:30.
  • Mikkel N. Lund: Standing on the shoulders of Dwarfs: the Kepler asteroseismic LEGACY sample I — oscillation mode parameters
    Updated: Wed 5th April 2017 15:02.
  • Zhao Guo: Tidally Induced Pulsations in Kepler Eclipsing Binary KIC 3230227
    Updated: Thu 23rd March 2017 09:48.
  • Kuldeep Verma: Seismic measurement of the locations of the base of convection zone and helium ionization zone for stars in the Kepler seismic LEGACY sample
    Updated: Wed 8th March 2017 11:56.
  • James M. Nemec: Metal-Rich SX Phe stars in the Kepler Field
    Updated: Wed 1st March 2017 07:53.

Kepler mission clock

Launch Countdown: